View allAll Photos Tagged Subframing
"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?
APEX 17x8.5" ET20 ARC-8 Wheels (4x100)
GC coilovers and camber is adjusted out on rear using adjustable subframe
Wheels: Race Silver EC-7
Front: 18x8.5 ET45
Rrear: 18x8.5 ET35
Additional notes:
E9X M3 subframe conversion including rear hubs (effective offset change)
Wheels: Race Silver EC-7
Front: 18x8.5 ET45
Rrear: 18x8.5 ET35
Additional notes:
E9X M3 subframe conversion including rear hubs (effective offset change)
Wheels: Race Silver EC-7
Front: 18x8.5 ET45
Rrear: 18x8.5 ET35
Additional notes:
E9X M3 subframe conversion including rear hubs (effective offset change)
Customer's preferred shop: @brintechcustoms
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: ç–; 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.
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.
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
Kosmo Foto Mono pushed to ISO400 - Nikon F3 - 100mm Series E f2.8
Home developed w/ Rodinal, home scanned.
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.
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.
Talk about a car that literally ruined everything!
The Lancia Beta had promise, it was very stylish and a very good car to drive, performing quite suitable when compared to other machines of similar class.
But once the honeymoon period was over, that's when the problems really sailed into port.
First off was the electrics. Lancia's have never been known for good electrics, and this car was no exception. But critically, the biggest problem was the rust. Show these cars a damp sponge and they'd start to whittle away.
Because of this, the company was laden with thousands of complaints and bad press about the poor conditions of the car. These problems have often been attributed to poor rustproofing techniques as well as the prolonged strikes that plagued Italy at that time rather than the metal's origin.
The corrosion problems could be structural; for instance where the subframe carrying the engine and gearbox was bolted to the underside of the car. The box section to which the rear of the subframe was mounted could corrode badly, causing the subframe to become loose. Although tales of subframes dropping out of vehicles were simply not true, a vehicle with a loose subframe would fail a technical inspection. In actuality, the problem affected almost exclusively 1st Series saloon models and not the Coupé, HPE, Spider or Montecarlo versions.
Eventually the circulation of bad press, thousands of Pounds of compensation and collection of recalls resulted in Lancia being forced to pull out of the British market in 1994, to which it hasn't returned.
Image from stacking
36x300s 3h
-Pre Processing-
Image Calibration
Cosmetic Correction
Debayer
Subframe Selector
Star Alignement
Local Normalization
Drizzle x2
Crop the black bands from the stacking
Owners of the BMW 3 Series (E46 models) have been reporting cracks and damage in the rear subframe area of their vehicles. The issue was also common on the earlier 3 Series models and unfortunately, have reoccurred with the E46 from 1999-2006. This issue specifically appears in the rear mounting points of the subframe, which can tear out from their position in the sheet metal. This occurs as the rear differential transmits the torsional load from the engine through the subframe, and then, into the chassis of the vehicle. This constant abuse leads to fatigue in the metal, causing cracks and separation from the chassis.
The parts used for this repair includes:
Active Autowerke (www.activeautowerke.com):
• E46 Subframe / Rear Chassis Reinforcement Kit
Powerflex USA (powerflexusa.com):
• BMW E46 M3 Rear Subframe Front Bushing - Street
• BMW E46 M3 Rear Subframe Rear Bushing - Street
• BMW E46 M3 Rear Diff Rear Mount - Street
• BMW E46 M3 Rear Diff Front Mount - Street
Owners of the BMW 3 Series (E46 models) have been reporting cracks and damage in the rear subframe area of their vehicles. The issue was also common on the earlier 3 Series models and unfortunately, have reoccurred with the E46 from 1999-2006. This issue specifically appears in the rear mounting points of the subframe, which can tear out from their position in the sheet metal. This occurs as the rear differential transmits the torsional load from the engine through the subframe, and then, into the chassis of the vehicle. This constant abuse leads to fatigue in the metal, causing cracks and separation from the chassis.
The parts used for this repair includes:
Active Autowerke (www.activeautowerke.com):
• E46 Subframe / Rear Chassis Reinforcement Kit
Powerflex USA (powerflexusa.com):
• BMW E46 M3 Rear Subframe Front Bushing - Street
• BMW E46 M3 Rear Subframe Rear Bushing - Street
• BMW E46 M3 Rear Diff Rear Mount - Street
• BMW E46 M3 Rear Diff Front Mount - Street
43x120 second subframes, iso800.
Total exposure 1 hour 26 minutes.
Modified Canon 350D (Baader ACF-2)
Takumar 200mm lens at F5.6 (with Astronomik CLS filter, in Cambridge)
Skywatcher Star Adventurer
Stacked and processed in DSS, Fitswork and Gimp
17th and 24th June 2017
Welney and Cambridge, UK
Fitted with a subframe for underfloor tipping gear.
Note the 22RB excavator in for repair in the background.
This factory is now the site of the new Oundle Waitrose.