View allAll Photos Tagged Subframing
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
To reduce engine movement a full set of engine, transmission and subframe mounts were installed. This results in less engine slop between shifts and smooth acceleration off the line.
Stock Subframe Mounts
Spoon Steering Rack Bushing Kit and Subframe Rigid Collar Kit: Convertible/Open Top car frames are generally weak. OEM's reinforce them to reduce chassis flex and twist. A torsionally weak frame will store suspension energy and release it in an uncontrolled manner. This results in less tire to road contact and unpredictable steering precision.
Lucky for us, Honda did an amazing job of engineering an 'x' frame by adding a backbone frame to tie the front and rear frame rails.
We opted for spoon rigid collars for the front and rear subframe because we've had positive results in other race cars we've built in the past. The subframe through holes are larger in diameter than their matching bolts. The large dimensional tolerances allow for the subframe to shift and bolts to flex. The Spoon rigid collars essentially fill up the "air space" gap if you will, so the amount of flex and shifting now becomes negligible. A primitive way to check for subframe shift is to simply add a couple of small tack welds between the subframe and chassis. An S2k equipped with slicks with 1 day of Buttonwillow testing will simply popped these welds. If not, you're either not driving hard enough or your welds are too large!
The OEM steering rack bushings are made of rubber. Due to the additional grip of running R comps and slicks we found a significant amount of steering play on previous S2000's. The data we collected shows the steering rack was shifting laterally resulting in unpredictable front toe change caused by rubber bushing deflection. Some S2000 enthusiasts assume the root cause is due to improper tie rod angle causing the front to 'bumpsteeer". Measuring front bumpsteer on lightly modded S2000's we find very small amounts of toe change through the swing arc. We can confidently say that most S2k enthusiasts don't need front BSK's however on Irene, we've done so much to the control arm angles, ride height and roll center geometry, adjustable solution is required so we used the Wicked Tuning Anti-Bumpsteer Kit to dial in the front. (REFER TO PHOTOS OF FRONT TIE RODS)
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
Hydragas spheres and brackets, and little cross member jobby, and the tin of paint. I hand brushed these, it went on quite thick and dried in a few minutes.
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
Target IC434 (Horsehead Nebula)
Camera SBIG STL-11000M CCD Camera
Subframe exposure 1200 seconds x 10 (3 hours & 20 minutes)
Focal Length 1043mm
Filter Hydrogen-Alpha 8nm
Telescope Astro-Physics AP 140 (140mm aperture)
Imaging Location Latitude +30:12:47.40, Longitude +081:36:04.20
Date Taken November 20, 2011 through November 25, 2011
ASTROMETRIC SOLUTION RESULTS
Center RA: 05h 41m 18.0s
Center Dec: -02° 21' 41.9"
Scale: 1.78 arcseconds/pixel
Size (pixels): 4008 x 2672
Angular Size: 1° 58' 50" x 1° 19' 13"
Position Angle: 261° 03' from North
RMS: 0.85 (X: 0.60 Y: 0.59)
Number of Stars Used in Solution: 382 (100%)
FWHM: 2.57 pixels, 4.57 arcseconds
Image Capture & Image Processing Jonathan Burnett
2020.04.18 Removing and patching up the subframe. Fixing a few rusty spots, and repaired the broken diff mount. Waiting now for subframe bushings and reassembly
25 September 2023, 01:53 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: Very faint ring visible in subframes.
from Stellarium:
Azimuth: 170°
Altitude: 42°
Magnitude: 7.6
Apparent size: 25 x 13 arcmin
Moon illuminated: 75%
Clouds: partly cloudy
Transparency: cloudy
Seeing: good
from Wikipedia
The Helix Nebula (also known as NGC 7293 or Caldwell 63) is a planetary nebula (PN) located in the constellation Aquarius. Discovered by Karl Ludwig Harding, most likely before 1824, this object is one of the closest of all the bright planetary nebulae to Earth. The distance, measured by the Gaia mission, is 655±13 light-years. It is similar in appearance to the Cat's Eye Nebula and the Ring Nebula, whose size, age, and physical characteristics are similar to the Dumbbell Nebula, varying only in its relative proximity and the appearance from the equatorial viewing angle. The Helix Nebula has sometimes been referred to as the "Eye of God" in pop culture, as well as the "Eye of Sauron".
The Helix Nebula is an example of a planetary nebula, formed by an intermediate to low-mass star, which sheds its outer layers near the end of its evolution. Gases from the star in the surrounding space appear, from our vantage point, as if we are looking down a helix structure. The remnant central stellar core, known as the central star (CS) of the planetary nebula, is destined to become a white dwarf star. The observed glow of the central star is so energetic that it causes the previously expelled gases to brightly fluoresce.
The nebula is in the constellation of Aquarius, and lies about 650 light-years away, spanning about 0.8 parsecs (2.5 light-years). Its age is estimated to be 10600+2300
−1200 years, based on the ratio of its size to its measured expansion rate of 31 km·s−1.
The Helix Nebula is thought to be shaped like a prolate spheroid with strong density concentrations toward the filled disk along the equatorial plane, whose major axis is inclined about 21° to 37° from our vantage point. The size of the inner disk is 8×19 arcmin in diameter (0.52 pc); the outer torus is 12×22 arcmin in diameter (0.77 pc); and the outer-most ring is about 25 arcmin in diameter (1.76 pc). The outer-most ring appears flattened on one side due to it colliding with the ambient interstellar medium.
Expansion of the whole planetary nebula structure is estimated to have occurred in the last 6,560 years, and 12,100 years for the inner disk. Spectroscopically, the outer ring's expansion rate is 40 km/s, and about 32 km/s for the inner disk.
The Helix Nebula was the first planetary nebula discovered to contain cometary knots. Its main ring contains knots of nebulosity, which have now been detected in several nearby planetary nebulae, especially those with a molecular envelope like the Ring nebula and the Dumbbell Nebula. These knots are radially symmetric (from the CS) and are described as "cometary", each centered on a core of neutral molecular gas and containing bright local photoionization fronts or cusps towards the central star and tails away from it. All tails extend away from the Planetary Nebula Nucleus (PNN) in a radial direction. Excluding the tails, each knot is approximately the size of the Solar System, while each of the cusp knots are optically thick due to Lyc photons from the CS. There are about 40,000 cometary knots in the Helix Nebula.
The knots are probably the result of Rayleigh-Taylor instability. The low density, high expansion velocity ionized inner nebula is accelerating the denser, slowly expanding, largely neutral material which had been shed earlier when the star was on the Asymptotic Giant Branch.
The excitation temperature varies across the Helix nebula. The rotational-vibrational temperature ranges from 1800 K in a cometary knot located in the inner region of the nebula are about 2.5'(arcmin) from the CS, and is calculated at about 900 K in the outer region at the distance of 5.6'.