View allAll Photos Tagged Subframing
All custom VRP (Verona Racing Parts) aluminium chassis, swingarm, gas tank, subframe/airbox.
Custom exhaust by MRP (Massaua Racing Pipe)
All custom VRP (Verona Racing Parts) aluminium chassis, swingarm, gas tank, subframe/airbox.
Note the VRP aluminium/subframe combo with much bigger airbox
VRP = Verona Racing Parts ( made by Carlo Verona / Italy)
VRP aluminium chassis for Honda CR 125 1989
VRP swingarm
VRP rear subframe with integrated airbox
VRP aluminium subframe
VRP gas tank with air channels
All custom VRP (Verona Racing Parts) aluminium chassis, swingarm, gas tank, subframe/airbox.
Custom barpad
Finally got round to replacing the rear springs, as I found this was quite challenging due to the design of the rear subframe on the S80.
Without a Youtube video and a certain spring compressor, it would be impossible to complete this task.
The ride has transformed, the rear is much tighter and also a bit lower (what I wanted). Happy days!
SKU / Type 956917
EAN 4251244608477
My wife's daily driver of seven years was recently diagnosed with a rusted subframe. It was a repair that we could have afforded, but at almost fifteen years old--and also having spent almost all of that time (we presume) in the midwest--the entire car is slowly turning to rust and it is not worth our time to get it repaired.
We had decided that we would try and sell the car on Craigslist, so we spent some time cleaning the car and getting it ready. Today was going to be the final push, getting it washed and taking photos of it and making up a listing. We washed the car at home, then decided to take it to Marathon to vacuum it out before finding a parking lot to take photos in. Even from the house to the gas station, the car was acting incredibly janky, and by the time we got it to our chosen parking lot and started taking photos of it, it wasn't long before we gave up--and decided to junk the car.
We drove it home and called Victory Auto Wreckers, who will be coming to tow it away tomorrow. Here are some photos of the beloved Cavalier for posterity's sake.
n 2191. 3 May 1999.
Shaftesbury & District's extended BEA Routemaster RMA-type, when reconstruction to the lengthened RME1 was well advanced. The rear subframe had been removed so that a cracked rear axle casing could be sent off for repair. Seen at the Shaftesbury yard in company with ex-London Transport Bristol LH/ECW saloons.
Captured 26 Nov 2021, 21:39 hrs ET, Springfield, VA, USA. Bortle 7 skies, Stellarvue SV80/9D doublet achromat refractor at f/5.68 (eff. fl 454mm), Orion Atlas AZ/EQ-G Pro mount. Mallincam DS10C camera, bin 1, exposure 120 seconds, gain 20, live stack of 20 subframes, dark and flat frames subtracted. Optolong LeNhance filter, UV/IR cut filter. Reprocessed in Siril and Photoshop on 14 June 2023.
Clouds: partly cloudy
Seeing: good
Transparency: good
Moon phase: 67%
FOV: 2.16 x 1.62 degrees before cropping.
Resolution: 2.1 arcsec/pixel.
Orientation: Up is Southwest.
Appearance: Dim nebulosity, adjacent bright star Gamma Cassiopeia. IC 59 is at 7 o'clock and IC 63 is at 10 o'clock.
From Stellarium:
IC 59 (a.k.a. Gamma Cas Nebula, LBN 620) is a reflection nebula. Magnitude +13.3, size 10 x 5 arcmin.
IC 63 (a.k.a. Ghost of Cassiopeia, LBN 622) is an HII region excited by Gamma Cas. Magnitude +13.3, size 10 x 3 arcmin.
From Wikipedia:
Gamma Cassiopeiae, Latinized from γ Cassiopeiae, is a star at the center of the distinctive "W" asterism in the northern circumpolar constellation of Cassiopeia. Although it is a fairly bright star with an apparent visual magnitude that varies from 1.6 to 3.0, it has no traditional Arabic or Latin name. It sometimes goes by the informal name Navi.
Gamma Cassiopeiae is a Be star, a variable star, and a binary star system. Based upon parallax measurements made by the Hipparcos satellite, it is located at a distance of roughly 550 light-years from Earth.
Gamma Cassiopeiae is an eruptive variable star, whose apparent magnitude changes irregularly between +1.6 and +3.0. It is the prototype of the class of Gamma Cassiopeiae variable stars. In the late 1930s it underwent what is described as a shell episode and the brightness increased to above magnitude +2.0, then dropped rapidly to +3.4. It has since been gradually brightening back to around +2.2. At maximum intensity, γ Cassiopeiae outshines both α Cassiopeiae (magnitude +2.25) and β Cassiopeiae (magnitude +2.3).
Gamma Cassiopeiae is a rapidly spinning star with a projected rotational velocity of 472 km s−1, giving it a pronounced equatorial bulge. When combined with the star's high luminosity, the result is the ejection of matter that forms a hot circumstellar disk of gas. The emissions and brightness variations are apparently caused by this "decretion disk".
The spectrum of this massive star matches a stellar classification of B0.5 IVe. A luminosity class of IV identifies it as a subgiant star that has reached a stage of its evolution where it is exhausting the supply of hydrogen in its core region and transforming into a giant star. The 'e' suffix is used for stars that show emission lines of hydrogen in the spectrum, caused in this case by the circumstellar disk. This places it among a category known as Be stars; in fact, the first such star ever to be so designated. It has 17 times the Sun's mass and is radiating as much energy as 34,000 Suns. At this rate of emission, the star has reached the end of its life as a late O-type main sequence star after a relatively brief 8 million years. The outer atmosphere has an intense effective temperature of 25,000 K, which is causing it to glow with a blue-white hue.
Gamma Cassiopeiae is the prototype of a small group of stellar sources of X-ray radiation that is about 10 times stronger than emitted from other B or Be stars. The character of the X-ray spectrum is Be thermal, possibly emitted from plasmas of temperatures up to least ten million kelvins, and shows very short term and long-term cycles. Historically, it has been held that these X-rays might be excited by matter originating from the star, from a hot wind or a disk around the star, accreting onto the surface of a degenerate companion, such as a white dwarf or neutron star. However, there are difficulties with either of these hypotheses. For example, it is not clear that enough matter can be accreted by a white dwarf, at the distance of the purported secondary star implied by the orbital period, sufficient to power an X-ray emission of nearly 1033 erg/s or 100 YW. A neutron star could easily power this X-ray flux, but X-ray emission from neutron stars is known to be non-thermal, and thus in apparent variance with the spectral properties.
Evidence suggests that the X-rays may be associated with the Be star itself or caused by some complex interaction between the star and surrounding decretion disk. One line of evidence is that the X-ray production is known to vary on both short and long time scales with respect to various UV line and continuum changes associated with a B star or with circumstellar matter close to the star. Moreover, the X-ray emissions exhibit long-term cycles that correlate with the light curves in the visible wavelengths.
Gamma Cassiopeiae exhibits characteristics consistent with a strong disordered magnetic field. No field can be measured directly from the Zeeman effect because of the star's rotation-broadened spectral lines. Instead, the presence of this field is inferred from a robust periodic signal of 1.21 days that suggests a magnetic field rooted on the rotating star's surface. The star's UV and optical spectral lines show ripples moving from blue to red over several hours, which indicates clouds of matter being held frozen over the star's surface by strong magnetic fields. This evidence suggests that a magnetic field from the star is interacting with the decretion disk, resulting in the X-ray emission. A disk dynamo has been advanced as a mechanism to explain this modulation of the X-rays. However, difficulties remain with this mechanism, among which is that there are no disk dynamos known to exist in other stars, rendering this behavior more difficult to analyze.
Gamma Cassiopeiae has two faint optical companions, listed in double star catalogues as components B and C. Star B is about 2 arc seconds distant and magnitude 11, and has a similar space velocity to the bright primary. Component C is magnitude 13, nearly an arc second distant.
Gamma Cassiopeiae A, the bright primary, is itself a spectroscopic binary with an orbital period of about 203.5 days and an eccentricity alternately reported as 0.26 and "near zero." The mass of the companion is believed to be about that of the Sun, but its nature is unclear. It has been proposed that it is a degenerate star or a hot helium star, but it seems unlikely that it is a normal star. Therefore, it is likely to be more evolved than the primary and to have transferred mass to it during an earlier stage of evolution.
The Chinese name Tsih, "the whip" (Chinese: 策; pinyin: cè), is commonly associated with this star. The name however originally referred to Kappa Cassiopeiae, and Gamma Cassiopeiae was just one of four horses pulling the chariot of legendary charioteer Wangliang. This representation was later changed to make Gamma the whip.
The star was used as an easily identifiable navigational reference point during space missions and American astronaut Virgil Ivan "Gus" Grissom nicknamed the star Navi after his own middle name spelled backwards.
Kosmo Foto Mono pushed to ISO400 - Nikon F3 - 100mm Series E f2.8
Home developed w/ Rodinal, home scanned.
Captured 16 May 2022, ~23:00 hrs ET, Springfield, VA, USA. Bortle 8 skies, Celestron 8 inch SCT at f/6.3 (eff. fl 1290mm), Orion Atlas AZ/EQ-G Pro mount. QHY 294M Pro camera @ -10C, bin 1, exposure 32 seconds, gain 3100, 11MP mode, stack of 20 subframes, no calibration frames used. Baader Luminance filter.
Clouds: clear
Seeing: avg
Transparency: avg
Moon phase: full
FOV: 36 x 33 arcmin.
Resolution: 1.0 arcsec/pixel.
Orientation: Up is West.
Appearance: Classic globular cluster.
Notes: Focused center FOV. Unguided.
From Wikipedia:
Messier 13 or M13, also designated NGC 6205 and sometimes called the Great Globular Cluster in Hercules or the Hercules Globular Cluster, is a globular cluster of several hundred thousand stars in the constellation of Hercules.
M13 was discovered by Edmond Halley in 1714, and cataloged by Charles Messier on June 1, 1764.
About one third of the way from Vega to Arcturus, four bright stars in Hercules form the Keystone asterism, the broad torso of the hero. M13 can be seen in this asterism 2⁄3 of the way north (by west) from Zeta to Eta Herculis. Although only telescopes with great light-gathering capability fully resolve the stars of the cluster, M13 may be visible to the naked eye depending on circumstances. With a low-power telescope, Messier 13 looks like a comet or fuzzy patch. The cluster is visible throughout the year from latitudes greater than 36 degrees north, with the longest visibility during Northern Hemisphere spring and summer.
With an apparent magnitude of 5.8, it is barely visible with the naked eye on clear nights. Its diameter is about 23 arcminutes and it is readily viewable in small telescopes.
In traditional binoculars, the Hercules Globular Cluster appears as a round patch of light. At least four inches of telescope aperture resolves stars in M13's outer extent as small pinpoints of light. However, only larger telescopes resolve stars further into the center of the cluster.
About 145 light-years in diameter, M13 is composed of several hundred thousand stars, the brightest of which is a red giant, the variable star V11, also known as V1554 Herculis, with an apparent visual magnitude of 11.95. M13 is 22,200–25,000 light-years away from Earth, and the globular cluster is one of over one hundred that orbit the center of the Milky Way.
Single stars in this globular cluster were first resolved in 1779. Compared to the stars in the neighborhood of the Sun, the stars of the M13 population are more than a hundred times more densely packed. They are so close together that they sometimes collide and produce new stars. The newly formed, young stars, so-called "blue stragglers", are particularly interesting to astronomers.
The 1974 Arecibo message, which contained encoded information about the human race, DNA, atomic numbers, Earth's position and other information, was beamed from the Arecibo Observatory radio telescope towards M13 as an experiment in contacting potential extraterrestrial civilizations in the cluster. The cluster will move through space during the transit time; opinions differ as to whether or not the cluster will be in a position to receive the message by the time that it arrives.
The last two variables (V63 and V64) were discovered from Spain in April 2021 and March 2022 respectively.
Test assembly of the major components of the rear subframe. The rear suspension and wheels will be bolted to this. The hole is for the rocket.
"It's just a truck" my wife tells me...
It was covered in yellow pine pollen, as all things in NC are about now. I despecked and 'canvas' textured it in Photoshop to hide that fact.
1955 Chevy 1st series 3100, Camaro subframe and 350/350 driveline.
Super Sharp Truck. For sale @ $8500 OBO. You contact me, but it's not mine.
Trivia question!
What's the difference between a '55 First Series and a '55 Second Series?
Now that I own an intervalometer, it's much easier to take lots of subframes over a long period of time (in fact, now I can do it while I'm on the couch watching TV). So I figured I would try "going deep" and see if I could image some galaxies - and why not, with Leo and Virgo high overhead this time of year?
I constructed this image over a period of several nights, as I'm a bit new to this type of astrophotography, and it took me some time to get proper flat and bias frames and get them all blended properly. I don't know who the first guy was to figure out the whys and hows of stacking, dark frames, flat frames, and bias frames, but he must've been a pretty smart guy. If you do this right, then camera-induced noise and artefacts are drastically reduced. One of the goals I had in making this image (besides making a nice image) was to see if it's actually possible to image dim objects like this with an Alt/Az mount (i.e., my Nexstar 8). It was very pleasing to know that it's possible - this really opens up the sky for me and my less-than-optimal equipment.
So here's the result... this image shows M65 & M66 in Leo. M65 (right) is a type Sa spiral galaxy, and as can be seen in this image, has a prominent dust lane and is close to being edge-on. M66 (left) is a type Sb spiral, and as can be seen here, has a prominent central bar, widely separated arms, and many clumps of dust. Both of these galaxies are about 36 million ly away.
I find it incredible that these "island universes", containing billions of stars, are so small and dim that it's a challenge to see and image them. No doubt there are guys up there trying to do the same thing with the Milky Way right now.
26x120 second subframes, total integration 52 minutes.
Imaging:
Skywatcher Evostar 150,
QHY163C with Astronomik CLS filter.
Guiding:
190mm focal length finder-guider,
Orion SSAG.
All on
Skywatcher HEQ5 Pro
Captured using SharpCap. Guided with PHD2.
Stacked and processed in DSS, Fitswork and Gimp. 2x drizzle applied.
20th July 2017
Cambridge, UK
Finally got round to replacing the rear springs, as I found this was quite challenging due to the design of the rear subframe on the S80.
Without a Youtube video and a certain spring compressor, it would be impossible to complete this task.
The ride has transformed, the rear is much tighter and also a bit lower (what I wanted). Happy days!
SKU / Type 956917
EAN 4251244608477
Test assembly of the major components of the rear subframe. The rear suspension and wheels will be bolted to this. The hole is for the rocket.
Exhibited alongside London Transport NHG 732P at the 1976 Commercial Motor Show were these front and rear suspension sub frames.
Bought a upgrade for the subframe. The polyurethane bushings are inserted into the rubber subframe bushings, which tightens them up and limit the movement in them.
Brand: Parts4Swedes
Partnr: 61430104PU
My wife's daily driver of seven years was recently diagnosed with a rusted subframe. It was a repair that we could have afforded, but at almost fifteen years old--and also having spent almost all of that time (we presume) in the midwest--the entire car is slowly turning to rust and it is not worth our time to get it repaired.
We had decided that we would try and sell the car on Craigslist, so we spent some time cleaning the car and getting it ready. Today was going to be the final push, getting it washed and taking photos of it and making up a listing. We washed the car at home, then decided to take it to Marathon to vacuum it out before finding a parking lot to take photos in. Even from the house to the gas station, the car was acting incredibly janky, and by the time we got it to our chosen parking lot and started taking photos of it, it wasn't long before we gave up--and decided to junk the car.
We drove it home and called Victory Auto Wreckers, who will be coming to tow it away tomorrow. Here are some photos of the beloved Cavalier for posterity's sake.