View allAll Photos Tagged Subframing
(nearly) complete rear subframe goes back under the car.
This is what it looked like a few months ago: www.flickr.com/photos/jynweythek/5443535641/in/photostream
Front subframe etc. Hubs and spindles already reconditioned, original springs in good condition, steering rack is good too.
Stacked from ten subframes. Taken in intense moonlight. The comet is a tiny fuzzball, slightly above centre of the image, seen in Gemini.
After a week of soaking that stubborn bolt in WD40 each night it still wouldn't budge so I dropped the car as low as I could get it as it was rocking on the axle stands when I tried to free the bolt.
Cut the body work away around the point where the trailing arm was bolted in and this allowed me to get a breaker bar in straight on the socket with no extensions (broke another adapter this morning).
With a steel pole over the breaker to get a bit more leverage the bolt finally gave out with an almighty shriek. I was going to have to get the angle grinder on it if this hadn't worked but really didn't want to risk damaging important bits
Het achterste subframe is het verste weg, en zat vreemd genoeg ook vol zand. De Mehari wordt momenteel bijeengehouden door de kabelboom ;-)
51x120 second subframes, iso800
Total exposure 1 hour 40 minutes
Imaged over 3 sessions (28th, 29th November and 4th December 2016)
William Optics ZenithStar II 80 ED
Nikon D5000
Skywatcher HEQ5 Pro
25 September 2023, 02:56 UT; Stuart, Florida USA (Bortle 6).
Celestron CPC Deluxe 1100 HD at f/10. Mallincam DS10C camera, bin 2x2, exposure 10s, Mono8 (?), gain 3000, stacked best 136 of 200 frames, Optolong L-eNhance filter, no guiding, dark and bias frames subtracted, sensor 29°C. Processed in Siril and PS.
Appearance: Faint ring visible in subframes.
from Stellarium:
Azimuth: °
Altitude: °
Magnitude:
Apparent size: arcmin
Moon illuminated: 75%
Clouds: partly cloudy
Transparency: cloudy
Seeing: good
from Wikipedia
The Ring Nebula (also catalogued as Messier 57, M57 and NGC 6720) is a planetary nebula in the northern constellation of Lyra. Such a nebula is formed when a star, during the last stages of its evolution before becoming a white dwarf, expels a vast luminous envelope of ionized gas into the surrounding interstellar space.
This nebula was discovered by the French astronomer Charles Messier while searching for comets in late January 1779. Messier's report of his independent discovery of Comet Bode reached fellow French astronomer Antoine Darquier de Pellepoix two weeks later, who then independently rediscovered the nebula while following the comet. Darquier later reported that it was "...as large as Jupiter and resembles a planet which is fading" (which may have contributed to the use of the persistent "planetary nebula" terminology). It would be entered into Messier's catalogue as the 57th object. Messier and German-born astronomer William Herschel speculated that the nebula was formed by multiple faint stars that were unresolvable with his telescope.
In 1800, German Count Friedrich von Hahn announced that he had discovered the faint central star at the heart of the nebula a few years earlier. He also noted that the interior of the ring had undergone changes, and said he could no longer find the central star. In 1864, English amateur astronomer William Huggins examined the spectra of multiple nebulae, discovering that some of these objects, including M57, displayed the spectra of bright emission lines characteristic of fluorescing glowing gases. Huggins concluded that most planetary nebulae were not composed of unresolved stars, as had been previously suspected, but were nebulosities. The nebula was first photographed by the Hungarian astronomer Eugene von Gothard in 1886.
M57 is found south of the bright star Vega, which forms the northwestern vertex of the Summer Triangle asterism. The nebula lies about 40% of the distance from Beta (β) to Gamma (γ) Lyrae, making it an easy target for amateur astronomers to find.
The nebula disk has an angular size of 1.5 × 1 arcminutes, making it too small to be resolved with 10×50 binoculars.[11] It is best observed using a telescope with an aperture of at least 20 cm (8 in), but even a 7.5 cm (3 in) telescope will reveal its elliptical ring shape. Using a UHC or OIII filter greatly enhances visual observation, particularly in light polluted areas. The interior hole can be resolved by a 10 cm (4 in) instrument at a magnification of 100×. Larger instruments will show a few darker zones on the eastern and western edges of the ring, and some faint nebulosity inside the disk. The central star, at magnitude 14.8, is difficult to spot.
M57 is 0.787 kpc (2,570 light-years) from Earth. It has a visual magnitude of 8.8 and a dimmer photographic magnitude, of 9.7. Photographs taken over a period of 50 years show the rate of nebula expansion is roughly 1 arcsecond per century, which corresponds to spectroscopic observations as 20–30 km/s. M57 is illuminated by a central white dwarf of 15.75v visual magnitude.
All the interior parts of this nebula have a blue-green tinge that is caused by the doubly ionized oxygen emission lines at 495.7 and 500.7 nm. These observed so-called "forbidden lines" occur only in conditions of very low density containing a few atoms per cubic centimeter. In the outer region of the ring, part of the reddish hue is caused by hydrogen emission at 656.3 nm, forming part of the Balmer series of lines. Forbidden lines of ionized nitrogen or N II contribute to the reddishness at 654.8 and 658.3 nm.
M57 is of the class of starburst nebulae known as bipolar, whose thick equatorial rings visibly extend the structure through its main axis of symmetry. It appears to be a prolate spheroid with strong concentrations of material along its equator. From Earth, the symmetrical axis is viewed at about 30°. Overall, the observed nebulosity has been currently estimated to be expanding for approximately 1,610 ± 240 years.
Structural studies find this planetary exhibits knots characterized by well developed symmetry. However, these are only silhouettes visible against the background emission of the nebula's equatorial ring. M57 may include internal N II emission lines located at the knots' tips that face the central star; however, most of these knots are neutral and appear only in extinction lines. Their existence shows they are probably only located closer to the ionization front than those found in the Lupus planetary IC 4406. Some of the knots do exhibit well-developed tails which are often detectable in optical thickness from the visual spectrum.
The central star was discovered by Hungarian astronomer Jenő Gothard on September 1, 1886, from images taken at his observatory in Herény, near Szombathely. Within the last two thousand years, the central star of the Ring Nebula has left the asymptotic giant branch after exhausting its supply of hydrogen fuel. Thus it no longer produces its energy through nuclear fusion and, in evolutionary terms, it is now becoming a compact white dwarf star.
The central star now consists primarily of carbon and oxygen with a thin outer envelope composed of lighter elements. Its mass is about 0.61–0.62 M☉, with a surface temperature of 125,000±5,000 K. Currently it is 200 times more luminous than the Sun, but its apparent magnitude is only +15.75.
all the aluminum subframe parts are put on using these aluminum 1/8' rivets. you drill the panel, then apply silicone to seal it to the frame, and then finally rivet the panel on.
The new subframe is finally bolted into position. Next I need to rebuild the radius arms and then move onto sorting the floorpans properly.
Heidts subframe with nice tubular a-arms and power rack and pinion steering. The wiring will be cleaned up soon.
Twee uur aan de auto werken en dit is wat er onder ligt. Rest in peace wordt al snel Rust in pieces...