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Maharlikan House - by JBulaong 2019 oil on canvas painting 24" X 32"
#Maharlika #precolonialPhilippines #precolonialPhilippinenipahouse #utopia #Ophir #islandsofgold #Chryse #indigenousarchitecture #JBulaong #oiloncanvas #PhilippineArchitecture #FilipinoHouse #painting #tropicalhouse #tropicalarchitecture #indigenousarchitecture #woodenhouse
Rajah Sulayman - oil on canvas 24" x 32" by JBulaong 2016
#RajahSulayman #KingofManila #Ophir #landofgold #chryse #Maharlika #oiloncanvas #painting #JBulaong
The emphasis of this painting is on gold jewelries and gilded items. The Spanish conquistadores, in search of gold, were awed by the opulence of the archipelago's society. From the rajah down to his constituents - they flaunted their heirlooms as if "gold is everywhere." Gold together with tattoo was the order of fashion.
This from 6 45 s SER files taken with a ZWO ASI224MC camera with 3x Barlow and a ZWO UV/IR cut filter through the C14 at Cerritos College. I used FIreCapture to take this data. SER files were used to create stacks of the best 26% of frames in AutoStakkert, and those stacks were processed in PixInsight. The resulting images were registered and derotated in WinJUPOS, with the result undergoing some final tweaks in GIMP.
Acidalia Planitia and Chryse Planitia are visible on the left side of the northern hemisphere below the north polar cap. There appears to be some weather just south of the polar cap toward the limb of the planet.
This image focuses on the mouth of Kasei Valles, as it transitions into Chryse Planitia. The region experienced extreme flooding billions of years ago, which has left its mark in this scene, as described in the associated image release.
The region was imaged by the High Resolution Stereo Camera on ESA’s Mars Express on 25 May 2016 during orbit 15714. The image is centred on 309ºE/27ºN and the ground resolution is about 15 m per pixel. It was created using data from the nadir channel, the field of view which is aligned perpendicular to the surface of Mars, and the camera’s colour channels. North is to the right.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
This perspective view looks from an unnamed crater at bottom right towards a 25 km-wide crater named Worcester Crater. The region sits at the mouth of Kasei Valles, where fierce floodwaters emptied into Chryse Planitia.
The image was generated using data from the high-resolution stereo camera on ESA’s Mars Express. This scene is part of the region imaged on 25 May 2016 during orbit 15714. The main image is centred on 309ºE/27ºN and the ground resolution is about 15 m per pixel. The view is looking approximately to the south.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
This oblique perspective view of the Mawrth Vallis region of Mars was generated from the digital terrain model and the nadir and colour channels of the High Resolution Stereo Camera on ESA’s Mars Express. It shows two large, interconnected, and highly eroded craters sitting on the boundary between the martian highlands and lowlands (in Chryse Planitia). The larger crater is some 75 km across, and the smaller one about 35 km across. This can be seen in more detail in the associated perspective view.
Credits: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
On July 20, 1976, at 8:12 a.m. EDT, NASA received the signal that the Viking Lander 1 successfully reached the Martian surface. This major milestone represented the first time the United States successfully landed a vehicle on the surface of Mars, collecting an overwhelming amount of data that would soon be used in future NASA missions. Upon touchdown, Viking 1 took its first picture of the dusty and rocky surface and relayed the historic image back to Earthlings eagerly awaiting its arrival. Viking 1, and later Viking Orbiter 2, collected an abundance of high-resolution imagery and scientific data, blazing a trail that will one day take humans to Mars.
This color image of the Martian surface in the Chryse area was taken by Viking Lander 1, looking southwest, about 15 minutes before sunset on the evening of Aug. 21. The sun is at an elevation angle of 3 or 4 degrees above the horizon and about 50 degrees clockwise from the right edge of the frame. Local topographic features are accentuated by the low lighting angle. A depression is seen near the center of the picture, just above the Lander’s leg support structure, which was not evident in previous pictures taken at higher sun angles. Just beyond the depression are large rocks about 30 centimeters (1 foot) across. The diffuse shadows are due to the sunlight that has been scattered by the dusty Martian atmosphere as a result of the long path length from the setting sun. Toward the horizon, several bright patches of bare bedrock are revealed.
For more information on the 40th anniversary of Viking, click here.
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These official NASA photographs are being made available for publication by news organizations and/or for personal use printing by the subject(s) of the photographs. The photographs may not be used in materials, advertisements, products, or promotions that in any way suggest approval or endorsement by NASA. All Images used must be credited. For information on usage rights, click here.
"Chrysès" - Terre cuite de Michel-Ange Slodtz (18ème siècle)
(Musée du Louvre)
Chrysès était un prêtre d'Apollon dans la ville de Chrysé en Troade.
The main science objective for this observation is to measure the cone’s size and shape and compare obtained values with other three fields of cones in other areas of Mars. Such a study may help to find out if small cones within these fields bear similarities or not, and hence if they have been formed by same process or not.
Image cutout is less than 5 km (under 3 mi) top to bottom and is 282 km (175 mi) above the surface. For full images including scale bars, visit the source link.
www.uahirise.org/ESP_065976_1990
NASA/JPL-Caltech/UArizona
Are these fascinating formations the result of faults or dikes? Aurorae Chaos is a region of chaos terrain on Mars at the eastern end of the outflow channels from Valles Marineris into Chryse Planitia.
The image cutout is less than 5 km (3 mi) across and the spacecraft altitude was 267 km (166 mi). For full images including scale bars, visit the source link.
www.uahirise.org/ESP_057022_1725
NASA/JPL-Caltech/UArizona
The pre-dawn morning of May 25th provided me with the most stable skies that I have experienced so far this year. The previous morning's Mars was a boiling sphere of red and no real details could be seen. But now the Red Planet wavered only mildly in my eyepiece at over 300-power, often showing sharpness rarely seen under my skies. The South Polar cap was pointed in Earth’s direction and was distinct (south is up in the drawing). Mare Erythraeum dominated the south while Mare Acidalium darkened the northern hemisphere, with the bright desert region of Chryse in-between. The Eye-of-Mars (Solis Lacus) appeared as a dark bump extending to the right of Mare Eryhraeum. I live for stable skies like I had the morning of May 25th. I only hope that such nights will continue to appear, on occasion, over my house as Mars grows in size over the next couple of months.
Additional Astronomical drawing can be seen at: www.orrastrodrawing.com
The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows a section of Ares Vallis. Numerous channels flow northward out of the Martian southern highlands and empty onto Chryse Planitia. These channels saw gigantic floods - as large or larger than any on Earth - early in Martian history. This was a time when Mars likely had a thicker atmosphere and a warmer climate. While Ares Vallis is not the widest or deepest outflow channel, it has a length of nearly 1,600 kilometers (1,000 miles).
The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial resolution and coverage of the image must be reduced to accommodate the additional data volume produced from using multiple filters. To make a color image, three of the five filter images (each in grayscale) are selected. Each is contrast enhanced and then converted to a red, green, or blue intensity image. These three images are then combined to produce a full color, single image. Because the THEMIS color filters don't span the full range of colors seen by the human eye, a color THEMIS image does not represent true color. Also, because each single-filter image is contrast enhanced before inclusion in the three-color image, the apparent color variation of the scene is exaggerated. Nevertheless, the color variation that does appear is representative of some change in color, however subtle, in the actual scene. Note that the long edges of THEMIS color images typically contain color artifacts that do not represent surface variation.
This martian scene spans 18 x 276 kilometers (11 x 171 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20250818a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
****THIS IMAGE HAS BEEN SUPERSEDED BY AN IMPROVED PROCESSING TECHNIQUE. SEE HERE FOR UPDATED IMAGE****
Mars Express view of Chryse Planitia and western Arabia Terra on February 23, 2015. This image was made from a two color (blue-green) observation of hazes in the atmosphere.
A seasonal dust cloud drifts above the southern edge of Chryse Planitia. Small local dust storms contributing to this dust cloud can be seen to its left. Meanwhile, the skies over western Arabia Terra and Margaritifer Terra were relatively dust-free.
This image was taken during Mars Express' 14,144th orbit of Mars.
Image Credit: ESA/DLR/FU Berlin/J. Cowart, CC BY-SA 3.0 IGO
Here's Mars from yesterday morning showing the dust storm blowing across Chryse (South is to the upper left). This image is from a single 4-minute video. 12.5" f/5.1 newtonian, 26mm Tele Vue Plossl, ZWO ASI662mc, UV/IR blocking filter.
“Viking I This is a color camera test strip on the Viking I lander’s color bars, this device helps calibrate the color TV camera for sending back true color of the Martian surface.”
Yet another well-crafted, thought out & succinct NASA description.
As a handful of the less than a handful of you that stumbled on this post might recall, the first published color Viking 1 lander photograph featured a blue sky. This was corrected and reissued a day or two later.
So, in this test photo – which shows the color calibration chart – the sky (taking into account the yellowing of the overall image) is definitely blue…at a minimum...‘bluish’. So, wouldn’t/shouldn’t that have been ‘caught’ in this image? I mean, if you get the colors right on the color calibration chart, wouldn’t that have automatically meant the rest of the colors in the image would also be correct, i.e., NOT blue??? I don’t get it.
Interesting:
www.donaldedavis.com/PARTS/MARSCLRS.html
Credit: “Don Davis: Space Artist and Animator” website
Also:
www.nasa.gov/mission_pages/msl/multimedia/pia16800.html
Finally, maybe the answer lies within the following, but I sure as hell ain’t reading the whole thing:
Note also the black grid pattern on the lander’s near pristine white surface, meant to gauge dust deposition both from the soil sampler depositing material in the experiment intakes on top of the lander deck and deposition by atmospheric dust. Earlier during this first Viking year on Mars, there were two great dust storms, the most intense lasting about 90 sols.
Today's VIS image shows a small section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. This channel, and all others in this region, drain into Chryse Planitia. Shalbatana Vallis is 1029km long (639 miles).
This martian scene spans 19 x 276 kilometers (12 x 171 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20250911a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Had good seeing about a week after the recent 2025 Mars opposition. North (top) and South Polar caps are evident as well as a number of identifiable geographical features / regions - Sinus Meridiani, Sinus Sabaeus, Arabia Terra, Mare Serpentis, Edge of Syrtis Major, Schiaparelli Crater, Chryse Planitia, Acidalia Planitia and more. Clouds can also be seen along the left limb. This is my best image of Mars. Looking ahead to the Red Planet's next opposition in 2027.
Date: January 23, 2025
Bortle Class 5 backyard, SF Bay Area (East Bay)
Capture: 5000 frames per filter, lucky imaging (FireCapture)
Telescope: Celestron C9.25 SCT
Camera: ZWO ASI462MM
Filters: Astronomik R,G,B
Tele Vue 2x Powermate
Mount: iOptron GEM45
Processing: AutoStakkert!4, waveSharp 2.0, Photoshop CC
Nombre del autor: Eduardo López.
Ciudad de origen y país: Caracas, Venezuela.
Dónde fue tomada la foto: En un sitio llamado El Mango, carretera Higuerote-Chirimena, cruce con la carretera a Curiepe, Barlovento, Estado Miranda, centro norte de Venezuela.
Contenido de la foto: Un Araguaney (Tabebuia chrysantha) en flor.
Por qué es especial: Porque es el árbol emblemático nacional de Venezuela y su día se celebra el último domingo de mayo.
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Lugar: El Mango, carretera Higuerote-Chirimena, cruce con la carretera a Curiepe, Barlovento, centro norte de Venezuela.
El día que tomé esta foto la Fila del Cabo resplandecía con el amarillo de cientos de araguaneyes en flor.
Una foto más cercana de las flores se puede encontrar aquí.
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Sobre nuestro árbol emblemático nacional he escrito el texto que sigue en el cual se refieren algunos de los atributos que se le asignan.
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Sin la menor duda el Araguaney (Tabebuia chrysantha), árbol loado, hoy como ayer, por muchos de los habitantes de Venezuela, ya tiene firmemente ganada y reconocida su posición descollante, no obstante las objeciones que hicieran en su momento Enrique Bernardo Núñez y otros (Núñez, 2005 [1932-1960], p. 79-81) a su selección como árbol emblemático nacional. Primero que nada, se trata de una especie que se da a lo largo y ancho de nuestra geografía, diseminádose por casi todas partes, como bien indicaba Antonio García Delepiani en el párrafo que se transcribe a continuación:
«La particularidad más resaltante del Araguaney consiste en su adaptación a todas las disímiles regiones del país: Crece silvestre en el llano y en la montaña; suele abrirse paso entre los gigantes de las selvas... Ningún otro de sus hermanos en la flora venezolana tiene esa generalidad nacional» (García, 1955, p. 66).
Ese carácter ubicuo del Araguaney que, fuera de la temporada de floración, tal vez pudiera pasar desapercibido para aquellos que no estén muy familiarizados con nuestra variadísima vegetación, se transforma en omnipresencia impactante durante los meses del verano, cuando se lo ve florecer por doquier como una marea de amarillo intenso imposible de ignorar. En palabras de Eleazar Orta «el araguaney es, sin duda alguna, uno de los árboles más bellos de nuestros bosques en el tiempo de su florescencia. Cubierto completamente con flores de un color amarillo dorado hermosísimo, constituye el más brillante espectáculo de magia y color de la naturaleza venezolana» (Orta, [Sin fecha], p. 2).
Otro hecho de la mayor relevancia es la identificación que parece existir en el inconsciente colectivo entre el Araguaney y las nociones de vitalidad, vigor y resurgencia, ya que su esplendorosa floración se produce precisamente entre los meses de febrero a abril, cuando la sequía arrecia haciendo que los campos y bosques castigados por ella parezcan desfallecer de tristeza y se vistan de luto a causa de los incendios forestales, como bien hacía notar el ya citado García Delepiani en el texto que sigue:
«El Araguaney es riqueza emotiva: sus expresiones embellecen nuestros campos en la época en que la sequía los tuesta y los afea. Son estos los meses en que el Arbol Nacional hace sentir su personalidad en la naturaleza del trópico venezolano. Se asoma a los paisajes para advertir que la vida subsiste dentro de la tierra cálida y sedienta; sus ramazones cubiertas de un vigor amarillo y el grito de las chicharras suplicando agua, son las tórridas señales de vida... Los campesinos lo aman en forma instintiva; es el poeta de los bosques cuando los bosques reclaman una esperanza tonificante» (García, 1955, p. 65-66). No es casual entonces que en la poesía de Pedro Lhaya, quien siempre se mantuvo enraizado con su pueblo, el Araguaney sea símbolo inapelable de la fortaleza y el aguante. Así lo dijo con suma claridad en La flor de Galipán, donde ponderó su resistencia a la sequía y al invierno en la estrofa siguiente:
«y de su terca savia de árbol múltiple,
amellador de hacha:
araguaney que permanece
contra la lengua ácida
de candelas de marzos, y aguas de noviembres.»
(Lhaya, 1967, p. 31)
Y, como era de esperarse, quien lucha, resiste y persiste sin llegar al desfallecimiento posee virtudes que son ante todo los adornos primordiales del araguaney, como bien se expresaba en la siguiente estrofa del poema Cimbrado Va, también del citado poeta barloventeño:
«Araguaney selvoso de veranos
me dio este duro nervio,
este cuerpo de Cristo rehuído
que se rebela al diente del murciélago.»
(Lhaya, 1963, p. 55)
Decía Jesús Hoyos que «aravenei parece ser la antigua voz con que el indio caribe denominaba al araguaney» (Hoyos, 1974, p. 23). Se trata de un «árbol autóctono, cuya altura oscila entre 6 a 12 metros» que posee una «madera de corazón durísimo y del color de la aceituna oscura. Se emplea en Venezuela, entre otras cosas, para hacer garrotes y bastones», lo mismo que las estacas llamadas laures con que se golpea en Barlovento el tronco del tambor mina, y a veces también a las personas en los jolgorios que terminan en riñas, lo cual explica que en otros tiempos fuera «muy frecuente oír que el araguaney truena y retumba en las espaldas, o abriendo las cabezas en canal» (Picón, 1964 [1912], p. 51).
El Araguaney «presenta un crecimiento lento, pero tiene una existencia larga», siendo el secreto de su ubicuidad, por una parte, su austeridad, que le permite prosperar en «suelos duros, secos, pobres en sustancias orgánicas» y, por la otra, que sus «semillas suelen estar maduras al comenzar las lluvias», fenómeno que permite «que el mayor número de semillas pueda germinar y perpetuar la especie a lo largo del tiempo» (Hoyos, 1974, p. 23), para el regocijo de los venezolanos de todas las épocas e inspiración de literatos y poetas, entre ellos ese apasionado por nuestra naturaleza que se llamara Jorge Schmidke, quien le compuso un soneto que dice:
«En la alta cumbre, en la cañada honda,
en el valle feraz y en la pradera,
para hospedar la núbil Primavera
alza el Araguaney su tienda blonda.
Con el Guarupa de cerúlea fronda
y el Bucare de cárdena cimera,
reproduce en los bosques la Bandera
que nos dió el paladín de la Gironda.
Su copa de amarilla vestidura
prende en la catedral de la espesura
su candelabro de doradas flamas;
porque la magia que su tronco encierra
chupa el oro del seno de la tierra
y lo presenta en flor sobre las ramas.»
(Schmidke, 1955, p. 16).
El género a que pertenece el Araguaney comprende otras especies parecidas con las cuales se pudiera confundir, ya que tienen también floraciones amarillas, aunque de tonalidades diversas, como son el Araguán o Cañada (Tabebuia chrysea), el Flor Amarilla, Curarí o Curarire (Tabebuia serratifolia) y el Acapro (Tabebuia tabilis) (Hoyos, 1987 [1983], p. 66 a 70), los cuales se pueden encontrar por aquí y por allá en Barlovento.
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Bibliografía citada
García Delepiani, Antonio. 1955. «Los meses del Araguaney». En: Schmidke, Jorge. 1955. «Breve antología del árbol. Poesías - Miscelánea». Ministerio de Agricultura y Cría. Caracas.
Hoyos, Jesús. 1974. «Arboles cultivados de Venezuela». Sociedad de Ciencias Naturales La Salle. Caracas.
Hoyos, Jesús. 1987 [1983]. «Guía de árboles de Venezuela». Sociedad de Ciencias Naturales La Salle. Caracas.
Lhaya, Pedro. 1963. «En medio de la tempestad». Ediciones Minotauro. Caracas.
Lhaya, Pedro. 1967. «La flor de Galipán». Ediciones del Cuatricentenario de Caracas. Caracas.
Núñez, Enrique Bernardo. 2005 [1932-1960]. «Arboles. Crónica de una ausencia. (Recopilación de Trino Borges)». Universidad de Los Andes. Mérida.
Orta, Eleazar. [Sin fecha]. «Emblemas naturales de Venezuela». Ministerio de Agricultura y Cría. Caracas.
Picón Febres, Gonzalo. 1964 [1912]. «Libro raro». Biblioteca de Autores y Temas Merideños. Mérida.
Schmidke, Jorge. 1955. «Breve antología del árbol. Poesía - Miscelánea». Ministerio de Agricultura y Cría. Caracas.
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This image shows part of the surface of Chryse Planitia, near the mouth of several of the giant outflow channels carved by massive floods. At this location the channel is much too large to be seen within a HiRISE image, and this shows an area of level plains near the mouth.
A long trough with aeolian (wind-blown) ripples runs through part of the image. This feature likely formed by contraction of the surface layer.
Image cutout is less than 1 km (under 1 mi) top to bottom and the spacecraft altitude was 284 km (176 mi). North is to the right. For full observation details including images with scale bars, visit the source link.
NASA/JPL-Caltech/UArizona
Acquisition date
12 January 2022
Local Mars time
15:34
Latitude (centered)
30.753°
Longitude (East)
321.003°
Spacecraft altitude
292.4 km (181.7 miles)
Original image scale range
59.7 cm/pixel (with 2 x 2 binning) so objects ~179 cm across are resolved
Source: www.uahirise.org/ESP_072492_2110
“COMING IN FOR A LANDING: This is artist Don Davis’ concept of how the Viking Lander, still enclosed in an aeroshell, will appear when it is some 20,000 feet above the surface of Mars as it prepares to land in July 1976. Two Viking spacecraft were launched in August and September from Cape Canaveral.”
And/or:
“This is artist Don Davis' conception of events some 20,000 feet above the Martin surface as the Viking lander (enclosed in a aeroshell) heads for a touch down on the plains of Chryse about July 4, 1976. After parachute deployment, the Viking lander detaches from the aeroshell and proceeds to a soft landing on the Martian surface, using small rockets for braking and maneuvering. The view is to the south. The bright star above the aeroshell is Fomalhaut. Capricorn is in the sky at right. The Mars landing will culminate a 704-million-kilometer journey from Earth which is scheduled to begin with launch on August 11, 1975. A second Viking will be launched 10 days later.”
Note, this beautiful work depicts actual Martian topography, and, as the second caption cursorily mentions (without context), that it's a view to the south. It’s looking across the original Viking 1 prime landing site, for crying out loud! Ugh.
You'd think that the “southerly view” would've been expounded on, instead of dwelling on what star & constellation are visible in the sky. If nothing else was going on, sure…attention to detail. 👍 And, all 3 - 5 of you know, I'm all about going down rabbit holes. In this case, the correct rabbit hole is obvious - and it doesn’t include Formalhaut & Capricorn. See the image below for the lacking context.
An amazing body of work, and much of it - in my world - iconic:
Credit: Don Davis: “Space Artist and Animator” website
This image shows a small portion of Mawrth Vallis, one of the many outflow channels feeding north into the Chryse Basin. This ancient valley once hosted flowing water. The erosive power of the flowing water rapidly cut down into the underlying layers of rock to expose a host of diverse geologic landforms visible today.
Intensely fractured bedrock is visible at all scales (meters to kilometers), revealing that subsurface rock has undergone a complex history of stresses and deformation, such as stretching, compression, and twisting.
Image is less than 1 km (less than 1 mi) across and is 285 km (177 mi) above the surface. For full image including scale bars and additional information, visit the source link.
www.uahirise.org/ESP_032125_2025
NASA/JPL/UArizona
"NASA 1970's Mars penetrator mission concept. The carrier spacecraft would launch the penetrator by rocket from a tube. An umbrella-like deployable fabric decelerator would be used to slow and stabilize the penetrator, which would leave an aftbody antenna at the surface."
The above, although associated with a black & white diagram of the image I've posted in the comments section, still aptly pertains to the striking view portrayed by Ken Hodges:
www.lpl.arizona.edu/~rlorenz/penetrators_asr.pdf
Credit: College of Science/Lunar & Planetary Laboratory/The University of Arizona website
AND!
“…A Mars Science Working Group (MSWG) chaired by Thomas Mutch was established by NASA to develop a science strategy for a future mission (Mars Science Working Group, 1977). It met four times in 1977. The plan assumed two Space Shuttle launches in December 1983 or January 1984, each carrying a spacecraft consisting of an orbiter, a lander with rover, and three penetrators, set to arrive at Mars in September or October 1984. The penetrators would be deployed just before arrival, but the rovers would wait in orbit until the dust storm season was over. Highly elliptical initial orbits would permit magnetospheric studies. After the rovers landed, the orbiters would enter circular orbits, one near-polar at 500 km altitude for global mapping and communication with the penetrators, the other 1000 km high with about a 30° inclination for rover communications. As the rovers might each deploy an instrument station with a seismometer, there could be ten simultaneously operating landed components.
As each orbiter neared the planet, it would deploy three penetrators which would fall on a circle around the centre of the planet’s disk as seen from the approach direction. After deployment the orbiters would be deflected off the approach path to enter orbit. The six penetrators, carrying seismometers and soil and atmospheric analysis equipment, would form a global array. Three would be placed about 500 km apart in an area likely to be seismically active, such as Tharsis. The other three would be spaced about 5000 km apart to give global coverage. Two additional and more sophisticated seismometers would be deployed by the rovers in areas partly shielded from the wind. Latitudes between 50° N and 87° S would be accessible, and the landing ellipses were 200-km-diameter circles. Slopes would have to be less than 45° at the impact point. Site selection was reported in a Penetrator Site Studies document preserved in Tim Mutch’s papers at Brown University. One potential array design was described (Table 36), along with four deployment options which include several additional sites (Table 37). Option 1 was the potential array described in Table 36. The penetrator sites in Table 37 were also described in Manning (1977), in which the site selection work was attributed to T. E. Bunch and Ronald Greeley.
The rover landing ellipses were roughly 50 by 80 km across. Five landing sites were studied using Viking data, in addition to the four sites previously considered by USGS for the Viking Rover (Figures 109 and 110). Only two sites were identified in the MSWG report, Capri and Candor (Table 38, Figures 111 and 112). The other sites were identified in Working Group documents among Tim Mutch’s papers in the archives at Brown University.
The rover landing ellipses in these documents were 65 by 40 km across. The polar orbiter would be able to deploy its rover from orbit at latitudes between 30° N and 50° N (this range could vary, depending on the launch date), whereas the low-inclination orbit could deliver a rover to latitudes between 20° S and 20° N.
Six rover landing sites were identified in a Rover Site Studies report prepared for the Working Group (Table 38a, Figure 111). Most derived from work done earlier for Viking or the Viking rover study, including proposals to land near Viking 1 and visit it or to explore the abandoned A-1 site with its complex geology. In a memorandum dated 9 May 1977, Hal Masursky followed up on discussions at a meeting of the Mars 1984 Mission Study Group held on 1 April. He asked Tim Mutch to request high-resolution stereoscopic Viking imaging coverage of four of these sites, using slightly different coordinates (Table 38b). These, he said, ‘were sites for which we have made traverse plans’. He added that ‘a backup smoother site near B-1’ at Cydonia had also been studied. Eventually the Capri and Candor sites were chosen, and detailed mission plans were prepared (Figure 109). Traverses near the Chryse sites were also prepared, including those in Figure 114.
The Capri site provided access to cratered uplands, crater ejecta and a fluvial channel. Candor was on the floor of the canyon system, with access to thick-layered deposits, canyon wall materials and, at the end of the extended mission, possibly the volcanic plateau surrounding the canyon. Alba had fractured volcanic plains and crater ejecta, but also small channels.
The Mars 1984 rovers had three traverse modes. Mode 1 was for detailed site investigations and involved only short, precise drives as needed for science operations. Mode 2, the ‘survey traverse mode’, would cover about 400 m per sol and could include some observations along the route. Mode 3, the ‘fast traverse mode’, could cover as much as 800 m per sol, including travel at night. The goal was to cover about 200 km during one Mars year and up to 200 km more in an extended mission in the second Mars year.
On 13 May 1977, Carl Pilcher, Hal Masursky and Ron Greeley suggested a variation on the role of penetrators in this mission. Two penetrators would be dropped in the lander target ellipse, carrying beacons to help guide the rover to a precision landing. After the landing they would operate with instruments on the lander itself as a local area seismic network.
The Mars 1984 orbiters would carry cameras, spectrometers for surface composition, infrared and microwave radiometers, a magnetometer, a plasma probe, a radar altimeter and communication relay equipment.
The relationship between Mars 1984 and other missions was considered by the Working Group. If Viking Lander 1 survived long enough, it might provide useful meteorological data for a Mars 1984 landing at Chryse, if that site was chosen. Conversely, Mars 1984 might be reconfigured to gather samples for collection by a sample return mission in about 1990.
Mars 1984 was not funded, probably in part because significant opposition to it arose in the science community. Jim Arnold and Mike Duke objected publicly that the final report of the Working Group did not reflect the group discussions, particularly in its assertions that the rovers were the only realistic option, that they were essential for future Mars Sample Return missions, and that simpler missions (orbiters, hard landers) were ‘a step backwards’. The report also suggested that only Mars rovers would command broad public interest, whereas missions such as Voyager, Jupiter Orbiter/Probe (Galileo) and the Lunar Polar Orbiter would not. This mention of Voyager refers to the outer planet spacecraft, not the earliest version of Viking (Table 2), and the suggestion that it would attract little public interest turned out to be the opposite of the truth. Elbert King (University of Houston) wrote to Mutch on 29 August 1977, stating emphatically that Mars 1984 ‘would only ensure a repeat of the very limited scientific success of Viking – providing mostly only costly clues and ambiguous answers to the important scientific questions’. He argued that only sample return was justified by the cost. This dismal assessment of Viking’s scientific worth stems from its failure to detect life, or to definitively rule it out, but overlooks its detailed characterization of surface and atmospheric composition, meteorology and landing site geology, not to mention the mission’s orbital data…”
WOW, I say again, WOW. The above phenomenal excerpt from “The International Atlas of Mars Exploration”, written by Philip J. Stooke, and most graciously made available by Cambridge Core/Cambridge University Press, at.
Wait one, maybe NOT so gracious.
Apparently, like everybody/place else, one is required to be registered or possibly possess an esteemed enough pedigree in order to be granted access...I apparently burned my one gratis peek:
www.cambridge.org/core/books/international-atlas-of-mars-...
We've come quite a way, eh? From dropping Jarts from orbit to flying a helicopter!
See also:
spaceflighthistory.blogspot.com/2017/08/prelude-to-mars-s...
spaceflighthistory.blogspot.com/2017/08/prelude-to-mars-s...
Both above credit: David S. F. Portree/"No Shortage of Dreams" blogspot
Last, but NOT least. This is a wonderful find, with a lot of fantastic imagery, to include this one. AND, it's still free, with no login/registration required...HOT-DAMN:
rpif.asu.edu/slides_mission_concepts/
Specifically:
rpif.asu.edu/slide_sets/future_mission_concepts/Mars_Pene...
Credit: Ronald Greeley Center for Planetary Studies/Arizona State University website
Mars Express HRSC image centered over Lunae Planum, a high-altitude plain northeast of Valles Marineris. This region has deep canyons carved out by large floods. These floods were probably created by the sudden melt of large reservoirs of subsurface ice. The release of this water caused the overlying materials to collapse, creating a jagged landscape appropriately called chaos terrain. These landscapes can be seen in the canyons at top right and center.
The outflow channels drain into the lowlands of Chryse Planitia. The channels carved by these floods terminate at remarkably similar elevations (within 200 m of each other), despite being separated by up to 2500 km. This has led some Martian geologists to infer the presence of an ancient ocean that once filled the planet's northern lowlands.
This natural color image was acquired by the Mars Express HRSC instrument during the spacecraft's 19,558th orbit of Mars, June 19, 2019.
Image Credit: ESA/DLR/FU Berlin/J. Cowart, CC BY-SA 3.0 IGO
The area of this very degraded crater is located along Maja Valles, a large system of ancient outflow channels that begins at Juventae Chasma (part of Valles Marineris) and ends in Chryse Planitia. The potential clays were detected by OMEGA, the spectro-imaging instrument of the ESA Mars Express mission, and this is a good example of coordination across missions to get better looks at the terrain when something interesting is noticed.
Image is less than 5 km (3 mi) across and is 273 km (169 mi) above the surface. For full images including scale bars, visit the below link.
NASA/JPL/UArizona
The colour-coded topographic view shows relative heights and depths of terrain in the region of Mars where Kasei Vallis reaches Chryse Planitia. As indicated in the key at top right, whites and reds represent the highest terrain, while blue is the lowest.
The image is based on a digital terrain model of the region, from which the topography of the landscape can be derived.
This region was imaged by the High Resolution Stereo Camera on ESA’s Mars Express on 25 May 2016 during orbit 15714. The image is centred on 309ºE/27ºN and the ground resolution is about 15 m per pixel. North is to the right.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
Rampart craters, also called fluidized-ejecta craters, have ejecta blankets that appear lobate, or rounded, and end in low ridges or ramparts, such as the ridge in this HiRISE image. Here you see the rampart at the edge of the ejecta blanket that comes from an approximately 16 kilometer (10 mile)-diameter crater to the east.
For years there has been a debate about whether these lobes and ramparts were formed by ejecta interacting with the thin Martian atmosphere, or whether they formed because volatiles (such as water or ice) in the subsurface were incorporated into the ejecta material excavated by the impact. The common consensus is now in favor of the volatile hypothesis. Because of this, rampart craters can be used to indicate the past presence of water or ice in the Martian crust.
Image is less than 5 km (3 mi) across and is 281 km (175 mi) above the surface. For full images including scale bars, visit the source link.
www.uahirise.org/ESP_014417_1975
NASAJPLUArizona
"NASA 1970's Mars penetrator mission concept. The carrier spacecraft would launch the penetrator by rocket from a tube. An umbrella-like deployable fabric decelerator would be used to slow and stabilize the penetrator, which would leave an aftbody antenna at the surface."
The above, associated with a black & white diagram of the image, labeled as Fig. 7, at:
www.lpl.arizona.edu/~rlorenz/penetrators_asr.pdf
Credit: College of Science/Lunar & Planetary Laboratory/The University of Arizona website
AND!
“…A Mars Science Working Group (MSWG) chaired by Thomas Mutch was established by NASA to develop a science strategy for a future mission (Mars Science Working Group, 1977). It met four times in 1977. The plan assumed two Space Shuttle launches in December 1983 or January 1984, each carrying a spacecraft consisting of an orbiter, a lander with rover, and three penetrators, set to arrive at Mars in September or October 1984. The penetrators would be deployed just before arrival, but the rovers would wait in orbit until the dust storm season was over. Highly elliptical initial orbits would permit magnetospheric studies. After the rovers landed, the orbiters would enter circular orbits, one near-polar at 500 km altitude for global mapping and communication with the penetrators, the other 1000 km high with about a 30° inclination for rover communications. As the rovers might each deploy an instrument station with a seismometer, there could be ten simultaneously operating landed components.
As each orbiter neared the planet, it would deploy three penetrators which would fall on a circle around the centre of the planet’s disk as seen from the approach direction. After deployment the orbiters would be deflected off the approach path to enter orbit. The six penetrators, carrying seismometers and soil and atmospheric analysis equipment, would form a global array. Three would be placed about 500 km apart in an area likely to be seismically active, such as Tharsis. The other three would be spaced about 5000 km apart to give global coverage. Two additional and more sophisticated seismometers would be deployed by the rovers in areas partly shielded from the wind. Latitudes between 50° N and 87° S would be accessible, and the landing ellipses were 200-km-diameter circles. Slopes would have to be less than 45° at the impact point. Site selection was reported in a Penetrator Site Studies document preserved in Tim Mutch’s papers at Brown University. One potential array design was described (Table 36), along with four deployment options which include several additional sites (Table 37). Option 1 was the potential array described in Table 36. The penetrator sites in Table 37 were also described in Manning (1977), in which the site selection work was attributed to T. E. Bunch and Ronald Greeley.
The rover landing ellipses were roughly 50 by 80 km across. Five landing sites were studied using Viking data, in addition to the four sites previously considered by USGS for the Viking Rover (Figures 109 and 110). Only two sites were identified in the MSWG report, Capri and Candor (Table 38, Figures 111 and 112). The other sites were identified in Working Group documents among Tim Mutch’s papers in the archives at Brown University.
The rover landing ellipses in these documents were 65 by 40 km across. The polar orbiter would be able to deploy its rover from orbit at latitudes between 30° N and 50° N (this range could vary, depending on the launch date), whereas the low-inclination orbit could deliver a rover to latitudes between 20° S and 20° N.
Six rover landing sites were identified in a Rover Site Studies report prepared for the Working Group (Table 38a, Figure 111). Most derived from work done earlier for Viking or the Viking rover study, including proposals to land near Viking 1 and visit it or to explore the abandoned A-1 site with its complex geology. In a memorandum dated 9 May 1977, Hal Masursky followed up on discussions at a meeting of the Mars 1984 Mission Study Group held on 1 April. He asked Tim Mutch to request high-resolution stereoscopic Viking imaging coverage of four of these sites, using slightly different coordinates (Table 38b). These, he said, ‘were sites for which we have made traverse plans’. He added that ‘a backup smoother site near B-1’ at Cydonia had also been studied. Eventually the Capri and Candor sites were chosen, and detailed mission plans were prepared (Figure 109). Traverses near the Chryse sites were also prepared, including those in Figure 114.
The Capri site provided access to cratered uplands, crater ejecta and a fluvial channel. Candor was on the floor of the canyon system, with access to thick-layered deposits, canyon wall materials and, at the end of the extended mission, possibly the volcanic plateau surrounding the canyon. Alba had fractured volcanic plains and crater ejecta, but also small channels.
The Mars 1984 rovers had three traverse modes. Mode 1 was for detailed site investigations and involved only short, precise drives as needed for science operations. Mode 2, the ‘survey traverse mode’, would cover about 400 m per sol and could include some observations along the route. Mode 3, the ‘fast traverse mode’, could cover as much as 800 m per sol, including travel at night. The goal was to cover about 200 km during one Mars year and up to 200 km more in an extended mission in the second Mars year.
On 13 May 1977, Carl Pilcher, Hal Masursky and Ron Greeley suggested a variation on the role of penetrators in this mission. Two penetrators would be dropped in the lander target ellipse, carrying beacons to help guide the rover to a precision landing. After the landing they would operate with instruments on the lander itself as a local area seismic network.
The Mars 1984 orbiters would carry cameras, spectrometers for surface composition, infrared and microwave radiometers, a magnetometer, a plasma probe, a radar altimeter and communication relay equipment.
The relationship between Mars 1984 and other missions was considered by the Working Group. If Viking Lander 1 survived long enough, it might provide useful meteorological data for a Mars 1984 landing at Chryse, if that site was chosen. Conversely, Mars 1984 might be reconfigured to gather samples for collection by a sample return mission in about 1990.
Mars 1984 was not funded, probably in part because significant opposition to it arose in the science community. Jim Arnold and Mike Duke objected publicly that the final report of the Working Group did not reflect the group discussions, particularly in its assertions that the rovers were the only realistic option, that they were essential for future Mars Sample Return missions, and that simpler missions (orbiters, hard landers) were ‘a step backwards’. The report also suggested that only Mars rovers would command broad public interest, whereas missions such as Voyager, Jupiter Orbiter/Probe (Galileo) and the Lunar Polar Orbiter would not. This mention of Voyager refers to the outer planet spacecraft, not the earliest version of Viking (Table 2), and the suggestion that it would attract little public interest turned out to be the opposite of the truth. Elbert King (University of Houston) wrote to Mutch on 29 August 1977, stating emphatically that Mars 1984 ‘would only ensure a repeat of the very limited scientific success of Viking – providing mostly only costly clues and ambiguous answers to the important scientific questions’. He argued that only sample return was justified by the cost. This dismal assessment of Viking’s scientific worth stems from its failure to detect life, or to definitively rule it out, but overlooks its detailed characterization of surface and atmospheric composition, meteorology and landing site geology, not to mention the mission’s orbital data…”
WOW, I say again, WOW. The above phenomenal excerpt from “The International Atlas of Mars Exploration”, written by Philip J. Stooke, and most graciously made available by Cambridge Core/Cambridge University Press, at.
Wait one, maybe not so gracious. Apparently, like everybody/place else, one is required to be registered or possibly possess an esteemed enough pedigree in order to be granted access...I apparently burned my one gratis token on the above. Hmm, I wonder if the Indonesian document hosting website has it:
www.cambridge.org/core/books/international-atlas-of-mars-...
We've come quite a way, eh? From dropping Jarts from orbit to flying a helicopter!
Also:
spaceflighthistory.blogspot.com/2017/08/prelude-to-mars-s...
spaceflighthistory.blogspot.com/2017/08/prelude-to-mars-s...
Both above credit: David S. F. Portree/"No Shortage of Dreams" blogspot
Today's VIS image shows a landslide deposit in Tiu Valles. The impact that created the crater likely caused the landslide, either during the impact event or shortly after. Located in Margaritifer Terra, Tiu Valles is part of a large system of channels that arise from Vallis Marineris and flow northward to empty into Chryse Planitia. Tiu Valles is 1720km long (1069 miles).
This martian scene spans 18 x 67 kilometers (11 x 42 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20220308a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
This is Mars from just before midnight on 16 April. It was bright enough that I was able to get a 5x Powermate on it with my F10 12 inch SCT, an equivalent of F50 - normally I try to stay around F25 to F30 with Mars. It has enabled me to capture some subtle detail although the image is a tad washed out by the high magnification involved. Of particular note, the Southern Polar ice-cap, which on Mars is off-set and not opposite the Northern Polar ice-cap, can be seen expanding into this image with Mars's North Pole still tilted towards the Earth. Syrtis Major is just moving round on the right edge, while the area known as Arabia hlds centre stage. The dark area to upper left is Acidalia with Chryse underneath. The dark region in central lower shot is Meridiani. Peter
Chryse Planitia (Greek for “golden plain”) is one of the lowest regions on Mars, and is the bottom end for many outflow channels of the southern highlands as well as from Valles Marineris.
NASA/JPL/UArizona
This pair of NASA/ESA Hubble Space Telescope images of Mars taken on 28 December (top) and 29 December (bottom) 2024. Each image shows a different side of the planet, with the accompanying moon Phobos. Various features are identified in the images, including the polar ice caps and clouds, as well as multiple terrestrial features.
At the midpoint of the observations, Mars was approximately 98 million kilometres from Earth. Thin water-ice clouds that are apparent in ultraviolet light give the Red Planet a frosty appearance. The icy northern polar cap was experiencing the start of Martian spring.
In the top image, the bright orange Tharsis plateau is visible with its chain of dormant volcanoes. The largest volcano, Olympus Mons, pokes above the clouds at the 10 o’clock position near the northwest limb. At an elevation of over 21 000 meters, it is 2.5 times the height of Mt. Everest above sea level. Valles Marineris, Mars’ over 4,000-kilometre-long canyon system, is a dark, linear, horizontal feature near center left.
In the bottom image, high-altitude evening clouds can be seen along the planet’s eastern limb. The 2,250-kilometre-wide Hellas basin, an ancient asteroid impact feature, appears far to the south. Most of the hemisphere is dominated by the classical “shark fin” feature, Syrtis Major.
[Image description: Two views of Mars. Top left text: Mars & Phobos, Hubble Space Telescope; filters in colors: F275W, purple; F410M, blue; F502N, green; F673N, red. Top image: December 28, 2024 20:00 UT. Most of the planet is shades of orange. The brightest orange area on the left half. At the top and bottom, white polar caps. Limb is blue. Text top center: northern polar cap, clouds. On planet, top to bottom, left to right: Arcadia Planitia, Tempe Terra, Acidalia Planitia; Olympus Monds; Tharsis Montes, Chryse Planitia; Valles Marineris, Terra Meridiana; Solus Planum; Argyre Planitia, Noachis Terra. To the right, dot: Phobos. Lower image: December 29, 2024 13:18 UT. Compass arrows at right, north pointing up, = east left. The planet has similar features; the brightest orange area is two centered two blobs. Text above Mars: northern polar cap, clouds. On-planet: Utopia Planitia; Arabia Terra, Syrtis Major; Terra Meridiani, Schiaparelli Crater, clouds; Noachis Terra, Huygens Crater, Syrtis Minor; Hellas Planitia. At left, dot: Phobos.]
Credits: NASA, ESA, STScI; CC BY 4.0
This context image shows a region of Mars where Kasei Vallis empties into the vast Chryse Planitia. The region outlined by the large white box indicates the area imaged during Mars Express orbit 15714, with the smaller inner box highlighted in an associated image release. In this context image, north is up.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
“VIKING DIGS A DEEP HOLE ON MARS -- This 110-degree color panorama of the Viking 1 Landing area was taken Feb. 17 to document deep-trenching activities that took place Feb. 12 and 14. The area viewed extends from north to northeast of the lander. The trench, to the right of the meteorology boom, is being dug to obtain samples from as far as 30 centimeters (12 inches) below the surface. Some significant changes can be seen in this picture, compared with earlier pictures of the landing area: the sky is much brighter than it was in the days just after landing last July. That indicates that the amount of dust suspended in the atmosphere has increased markedly, as more scattered light is now reaching the surface; hence the shadows (of the meteorology boom and the spacecraft itself) are no longer dark. Finally, the amount of reddish dust on the spacecraft has increased as a result of sampling activity: fine dust can be seen on the leg support and the radioisotope thermoelectric generator cover. On March 12 the surface sampler will deliver some fine material from the trench to the inorganic chemical instrument. That sample analysis may help explain the anomalously high sulfur content of previous samples. On April 2 a sample from the bottom of the trench will be delivered to the biology instrument so scientists can try to better understand the chemistry of the Martian soil observed in earlier experiments.”
While a whole lot of entities have, or offer this image - the JPL Photojournal website not being one of them - the following is the only one I came across that at least has an abridged version of the original caption:
www.tsgc.utexas.edu/spacecraft/viking/v1l_01.html
Credit: Texas Space Grant Consortium website.
"This color picture of Mars was taken July 21--the day following Viking 1's successful landing on the planet. The local time on Mars is approximately noon. The view is southeast from the Viking. Orange-red surface materials cover most of the surface, apparently forming a thin veneer over darker bedrock exposed in patches, as in the lower right. The reddish surface materials may be limonite (hydrated ferric oxide). Such weathering products form on Earth in the presence of water and an oxidizing atmosphere. The sky has a reddish cast, probably due to scattering and reflection from reddish sediment suspended in the lower atmosphere. The scene was scanned three times by the spacecraft's camera number no. 2, through a different color filter each time. To assist in balancing the colors, a second picture was taken of a test chart mounted on the rear of the spacecraft. Color data for these patches were adjusted until the patches were an appropriate color of gray. The same calibration was then used for the entire scene. Another version of this photo (Viking 1-46) with a sky that appeared more pink, gray and blue, was shown last week. This interpretation has been modified with further processing."
This photograph is in amazing condition. I'm serious, no hype. It's strikingly pristine.
www.nbcnews.com/news/amp/ncna314601
Credit: NBC News website
www.jpl.nasa.gov/spaceimages/details.php?id=PIA00563
Credit: JPL website
photojournal.jpl.nasa.gov/catalog/PIA00563
Credit: JPL photojournal website
Boston MFA 13.186 Skyphos Side B
******************************************************************************
Side B: Menelaos attacking Helen. On the right, Menelaos rushes at Helen with his head lowered, about to draw his sword. Helen flees to the left, turning back towards Menelaos. Menelaos is in full armor, with a short chiton, leather corslet, greaves, Attic helmet and a shield. The knees of the greaves are ornamented with gorgoneia, and a pad is tied around his ankle to keep the greaves from chafing. The corslet is strengthened with metal scales, and its shoulder-flap is decorated with a star. The shield, shown in front view rather than foreshortened, has a charging bull as a device. Helen turns back towards Menelaos, and extends her left arm towards him, and holds up her himation with her right. She wears a veil and stephane, necklace and earring.
Behind Helen, Aphrodite approaches, turning Helen's head towards her husband to still his anger. She wears a chiton and himation, earrings and a sakkos, and extends her arm out towards Helen. To the left of Aphrodite is another woman, looking round towards the scene and holding a flower. She wears a chiton with overfall, a girdle, a himation over both shoulders, a necklace and earrings. She is labelled Kriseis. Next to her is an old man, labelled Kriseus with a long white beard and white hair bound up with a cord. He wears a long chiton and himation, and holds a staff in his right hand. These two figures may be variant spellings of Chryses and Chryseis, the priest of Apollo and his daughter, with which the quarrel between Achilles and Agamemnon in the Iliad begins. The figures are all labelled.
Under both handles are figures. Under one, Priam sits on a folding stool covered with a checkered cloth, looking towards Menelaos and Helen. He wears a long chiton and himation, and holds a staff in his right hand and makes an apprehensive gesture with his left. He is bearded and the top of his head is bald, with his front hair tied in a knot in the middle of his forehead. Under the other handle is a small boy in a himation, stepping forwards towards Peitho on side A. He is unlabelled, but may be Helen's son whom she abandoned to follow Alexandros.
*******************************************************************************
Furtwaengler, Adolf ; Reichhold, Karl
Griechische Vasenmalerei: Auswahl hervorragender Vasenbilder; (Serie II, Tafel 61-120)
München 1909; Tafel 85
"Chrysès" - Terre cuite de Michel-Ange Slodtz (18ème siècle)
(Musée du Louvre)
Chrysès était un prêtre d'Apollon dans la ville de Chrysé en Troade.
“This is an artist’s concept of a 360 panorama of the planet Mars and the upper surface of the Viking lander as viewed by Camera No. 2”
I believe it’s the Viking 1 lander. A very rarely seen work by the immensely talented, knowledgeable & multifaceted Paul Fjeld:
www.hq.nasa.gov/alsj/fjeld.html
Credit: “Paul Fjeld: “SPACE ART By PAUL FJELD” website
If indeed Viking 1, compare/contrast:
photojournal.jpl.nasa.gov/catalog/PIA03166
Credit: JPL Photojournal website
“This mosaic of five Mars pictures shows the eastern part of the Chryse region near the prime Viking 1 landing site. The Viking Orbiter cameras took the pictures from a range of about 1600 kilometers (992 miles) on June 23. Braided channels record water flowing on the planet in the past. Fine grooves and hollows on the upstream side of flow obstacles also are seen. Shore of the channel is at lower right.”
To me, this was the most iconic/memorable early Viking Orbiter image that provided evidence of past flowing water on Mars.
And/or:
"Islands near Chryse Planitia
"Islands" near Chryse Planitia. Teardrop-shaped "islands" are shown at the mouth of Ares Vallis near the southern boundary of Chryse Planitia. Flow was from the south and apparently diverged around obstacles such as craters and low hills to form a sharp prow upstream and an elongate tail downstream. A shallow moat surrounds the entire island. Similar patterns on Earth have been formed by catastrophic floods, wind erosion, and glacial action. From top to bottom, the three large craters are named Lod, Bok, and Gold. [211-4987; 21°N, 31°W]"
Per:
"NASA SP-441: VIKING ORBITER VIEWS OF MARS". At:
history.nasa.gov/SP-441/ch4.htm
Specifically:
“This is a close-up of the sunset on Sol 24 as seen by the Imager for Mars Pathfinder. The red sky in the background and the blue around the Sun are approximately as they would appear to the human eye. The color of the Sun itself is not correct -- the Sun was overexposed in each of the 3 color images that were used to make this picture. The true color of the Sun itself may be near white or slightly bluish.
August 28, 1997
Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is a division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator.
Photojournal note: Sojourner spent 83 days of a planned seven-day mission exploring the Martian terrain, acquiring images, and taking chemical, atmospheric and other measurements. The final data transmission received from Pathfinder was at 10:23 UTC on September 27, 1997. Although mission managers tried to restore full communications during the following five months, the successful mission was terminated on March 10, 1998.”
The above & image at/from:
photojournal.jpl.nasa.gov/catalog/PIA00920
Credit: JPL Photojournal website
And, associated with the panoramic image of which PIA00920 is a portion:
“This image of the Martian sunset from Sol 24 shows much more color variation than had previously been seen. The blue color near the Sun is not caused by clouds of water ice, but by the Martian dust itself. The dust in the atmosphere absorbs blue light, giving the sky its red color, but it also scatters some of the blue light into the area just around the Sun because of its size. The blue color only becomes apparent near sunrise and sunset, when the light has to pass through the largest amount of dust. This image was taken by the Imager for Mars Pathfinder.”
Above & panorama at/from:
photojournal.jpl.nasa.gov/catalog/PIA01547
photojournal.jpl.nasa.gov/catalog/PIA00917
Both above credit: JPL Photojournal website
Remarkably & unfortunately, this is the FIRST Pathfinder inflight image - on photographic paper - that I’ve come across. Dang…that’s since 1997!
This might be the first image taken from the Martian surface of the solar disk at sunset. Although the Viking Landers took spectacular images of the sunset, to the best of my recollection, they were all after the sun was below the horizon. Although, the Viking 2 Lander did capture a sunrise:
photojournal.jpl.nasa.gov/catalog/PIA00576
Credit: JPL Photojournal website
And by Viking 1, also a sunrise:
www.planetary.org/space-images/sunrise-at-the-viking-1-la...
Credit: “The Planetary Society” website
"Chrysès" - Terre cuite de Michel-Ange Slodtz (18ème siècle)
(Musée du Louvre)
Chrysès était un prêtre d'Apollon dans la ville de Chrysé en Troade.
Hamelin Crater
This image straddles Hamelin with another crater, which is only 90 km northeast of the original landing site selected for Viking Lander 1 in Chryse Planitia. Hamelin shows the raised edge or rampart around the ejecta blanket that is characteristic of many craters in this area.
NASA/JPL/University of Arizona (284 km above the surface, less than x km top to bottom and north is to the right.)
Source: www.uahirise.org/ESP_020904_2005
“This is artist Don Davis' conception of the Viking Mars lander as it heads for a touch down on the Martian surface at the prime landing site, Chryse, about July 4, 1976. The view is to the west, with Earth about 20 degrees below the Sun. Parachute in left background carries the aeroshell from which the lander detaches at a distance of about 20,000 feet from the surface. The Mars landing will culminate a 704-million-kilometer (440-million-mile) Viking journey from Earth which is scheduled to begin with launch on August 11, 1975.”
And/or:
“Captured here in this rendering is a Viking lander just before it touched down on the Martian surface. The parachute and upper aeroshell can be seen in the upper left corner of the image. At this stage of the descent, the lander's terminal descent propulsion system (three retro-engines) had slowed the craft down so that velocity at landing was about of 2 meters per second (7 mph). Seconds after the lander reached the surface it began transmitting images back to the orbiter for relay to Earth.”
At:
www.tsgc.utexas.edu/spacecraft/viking/land2.html
Credit: Texas Space Grant Consortium website
“Color-enhanced image of sunset on Mars, recorded by the Viking 1 lander. Part of the spacecraft is just visible at bottom right, colored dark blue. The contouring effect around the setting sun is a result of the imaging system.”
Disappointingly, the image and the above, which may have been part of the original NASA caption, seem to only be available at the ‘pay to play’ sites.
A high contrast version is contained within:
history.nasa.gov/EP-177/ch8-2.html
Although I can see how this has an artistic, mod/pop…whatever it’s called, appeal, I’ve always disliked it. Yet it seemed to have been oft-reproduced. I remember seeing it as a poster, lithograph of course…I think even in NASA/JPL informational/promotional material.
It definitely looks way better as an actual photograph print, not the garish, ‘HDR’, end of “2001: A Space Odyssey”, comic book-like look I seem to recall & refer to above.
i.discogs.com/kAPI00d2TdTseTZwVL5YXOR03oD9osbsjRzeG_z1zbk...
i.discogs.com/Lc1xLVGuQIhLAr66dCTnXmd-qAXxrQPVuiUYqO3HBOU...
Credit: Both above credit Discogs website
Further, although the image is subdued & accurate, the ‘contour lines’ do seem to match. Maybe just processed differently? IDK:
“Viking 1 Lander image of a Martian sunset over Chryse Planitia. In this image the sun is 2 degrees below the local horizon. The banding in the sky is an artifact produced by the incremental brightness levels of the camera. This image was taken on the 30th Martian day (sol) after touchdown, at 19:13 local time. The camera is pointing towards the southwest.”
At:
nssdc.gsfc.nasa.gov/imgcat/html/object_page/vl1_12a240.html
Credit: NSSDCA website
Also:
commons.wikimedia.org/wiki/File:Viking_sunset.jpg
Credit: Wikimedia Commons
Finally, featured on the cover. The right half of it that is: