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Topic: Main-belt

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Asteroid belt - Wikipedia, the free encyclopedia Image of the main asteroid belt between the orbits of Mars and Jupiter. It is termed the main belt when contrasted with other concentrations of minor planets, since these may also be termed asteroid belts. Asteroid belts are a staple of science fiction stories less concerned with realism than with drama, since they are always portrayed as being so dense that adventurous measures must be taken to avoid an impact. en.wikipedia.org /wiki/Main_belt

main asteroid belt The main asteroid belt extends from 2.15 to 3.3 astronomical units (255 to 600 million km) from the Sun &; between Mars (1.5 AU) and Jupiter (5.2 AU) — and may contain over a million objects bigger than 1 km across, the largest being Ceres (1,003 km), Pallas (608 km), and Vesta (538 km). Within the belt, the distribution of asteroids is non-uniform, with concentrations in asteroid groups and families, and also relatively empty zones known as Kirkwood gaps. The belt appears to have originated as a system of perhaps 50 large bodies in the 100 to 1,000 km size range. www.daviddarling.info /encyclopedia/M/mainasterbelt.html

Safety belt for motor vehicle - Patent 4098524 Also belts equipped with a self-rolling device are practically impossible to be fitted in the rear of the vehicle because the self-rolling device must be situated in the same vertical line as the upper anchoring point, at a point where the embossing for the wheel passages prevents its installation. This belt comprises an auxiliary strap 8 constituted by a cable which is secured to the bottom of the body of the vehicle or to a side member of the frame thereof through the medium of a self-rolling device. Such types of belts all have numerous drawbacks, especially owing to the fact that the strap is doubled at the point where it can be unfastened, which condition frequently leads to its entanglement when the belt is not in service. www.freepatentsonline.com /4098524.html

Asteroids Between the main concentrations of asteroids in the Main Belt are relatively empty regions known as the Kirkwood gaps. The composition of these objects is probably more like that of comets or the Kuiper Belt objects than that of ordinary asteroids. These are regions where an object's orbital period would be a simple fraction of that of Jupiter. seds.lpl.arizona.edu /nineplanets/nineplanets/asteroids.html

Mine Safety and Health Administration (MSHA) - Coal Mine Fatal Accident Investigation Report: Fatality #8 - February 22, 2004 Powered Haulage - Underground - AL - Jim Walter Resources, Inc. - No. 7 Mine As a result, a miner contacted the moving belt conveyor while attempting to perform assigned belt maintenance, that included removing blockages, and was fatally injured as he contacted the moving belt or as he was subsequently transported on the belt 9000 feet through belt transfers and a rock breaker to the surface mine refuse pile. When the West "A" belt conveyor restarted and failed to clear the chute obstruction, the victim may have walked to the end of the catwalk, on the east side of the North Main head roller structure, and attempted to lean over the operating belt to thrust a 7-foot drill steel up the chute discharge. When this action failed, the victim may have crossed under the North Main belt conveyor to the east side, walked to the end of the east catwalk and positioned himself over the north edge of the moving West "A" belt conveyor to clear the obstruction with a 7-foot drill steel. www.msha.gov /FATALS/2004/FTL04c08.HTM

[6.04] The Fossilized Size Distribution of the Main Asteroid Belt During the planet formation epoch, the primordial main belt (PMB) contained several Earth masses of material, enough to allow the asteroids to accrete on relatively short timescales (e.g., Weidenschilling 1977). This period of comminution and dynamical evolution in the PMB created, among other things, the main belt's wavy size-frequency distribution, such that it can be considered a "fossil" from this violent early epoch. We will show that the constraints provided by asteroid families and the shape of the main belt size distribution are essential to obtaining a unique solution from our model's initial conditions. www.aas.org /publications/baas/v36n2/dda04/42.htm

Main V-belt Drive The RotorWay main power transmission mechanism from the engine to the secondary shaft is by means of eight "3V" section V-belts (3V-630), with each pair banded together into belted sets. The effective torsional rate of the belt drive is the applied torque divided by the angular deflection of the driving pulley caused by the belt stretch. Belts (and chains and pretty much everything else) stretch when a tension force is applied to them. www.epi-eng.com /RW-Vbelt.htm

Code Development to Model Collisional and Dynamical Evolution of the Main Asteroid Belt, 15-9360 Because material drained from the main belt becomes part of the steady-state NEO population, we can use NEO observations and terrestrial/lunar impact data to constrain the main belt population over size ranges where main belt data are currently unavailable. It is our intention to use this integrated "one-dimensional" model to predict the nature of the main belt and NEO size distributions from several different tens of micrometers to asteroid 1 Ceres. For these reasons, we believe that deriving the size-frequency distribution of the main belt and NEO populations is an essential component of the NASA research program. www.swri.org /3pubs/IRD2003/Synopses/159360.htm

Exploring Main Belt Asteroids - Draft White paper - NRC Decadal Study SpaceRef - Your Space Reference Today, main belt asteroids consist of a few unshattered protoplanets (e.g., Ceres, Pallas, Vesta) and disrupted protoplanets whose pieces were shattered and dispersed, then further shattered and dispersed leaving the hundreds of thousands of fragments that dominate the main asteroid belt today (e.g., Eros, Gaspra, Ida). For instance, the efficiency at which asteroids of given sizes from given (compositional) regions are removed from the main belt into near-earth orbits is useful as is the growth and physical properties of regolith of carbonaceous to metallic objects. The pursuit of basic science in the main asteroid belt may provide information that is useful to the utilization of asteroids in near-earth orbits to support future human space activity. www.spaceref.com /news/viewsr.html?pid=3918

[14.08] Exploring Main Belt Asteroids Terrestrial planet formation in the main asteroid belt was interrupted when growing protoplanets became sufficiently massive to gravitationally perturb the local population, causing bodies to collide with increased energy, thus ending accretion and commencing fragmentation and disruption. Few of these protoplanets are thought to have survived unshattered (e.g., Ceres, Vesta, Pallas), leaving a main belt population dominated by fragments of fragments, and significantly depleted of mass as a consequence of dynamical scattering. Missions to specific main belt targets can provide important new insights and leverage new understanding of existing data, models, and theories, but target definition (and corresponding instrument complement) is critical and must be based on our existing knowledge of these very diverse objects. www.aas.org /publications/baas/v33n3/dps2001/502.htm

hardersen.txt The petrologic compositions of the orthopyroxenes on these asteroids suggest that their parent bodies were formed in regions of the main asteroid belt that experienced relatively reducing chemical conditions. Results: The four main asteroids from this work, 69 Hesperia, 110 Lydia, 201 Penelope and 216 Kleopatra, have all been found to exhibit weak spectral features in the 1- and 2-micron regions of their NIR spectra. Specifically, the Band I centers for these asteroids fall in the range from 0.90 to 0.93 microns and the Band II centers are in the range from 1.76 to 1.84 microns. www.ifa.hawaii.edu /colloquia/abstracts/hardersen.txt

lederhosen: construction--belts The belt may have some practical purposes, especially for Scouting as a variety of items can be attached to the belt. There appear to at least four options that are currently practiced: 1) no belt, 2) a belt worn without any attachment to the lederhosen, 3) a belt worn under the front part of the lederhosen, and 4) a belt worn with lederhosen belt loops. Some of these boys wear their lederhosen without either a halter or a belt. www.histclo.hispeed.com /style/casual/leder/lconst-belt.html

Business Wire: SwRI Researchers Identify Asteroid Breakup Even... @ HighBeam Research The main asteroid belt, a population of roaming boulders with sizes ranging from Texas-sized rocks to tiny pebbles, lies between the orbits of Mars and Jupiter. Because the Karin cluster asteroids could have been given "blank slates" 5.8 million years ago, craters formed since that time by asteroid collisions could be used to estimate the current crater production rate in the main belt. The known age of the Karin-cluster members also could help explain the rate at which asteroids strike one another in the main belt. www.highbeam.com /library/doc0.asp?DOCID=1G1:87134153&refid=holomed_1

First Triple Asteroid System Found The asteroid 87 Sylvia is one of the largest known from the asteroid main belt, which is located between the orbits of Mars and Jupiter. Seventeen of these binary systems are in the main asteroid belt and have been imaged directly either by adaptive optics systems on large, ground-based telescopes or by the Hubble Space Telescope. From two months' of observations of the moonlets' orbits, Marchis and his Paris colleagues were able to precisely calculate the mass and density of Sylvia, which shows it to be a "rubble-pile" asteroid, Marchis said. www.sciencedaily.com /releases/2005/08/050810135320.htm

New Clusters for highly inclined Main Belt Asteroids Figure 3: Main Belt asteroids: (e, sin i) distribution with (sin i) > 0.3 Phocaea region is clearly visible in the inner part of the Main Belt, with proper elements 2.2 0.3. Abstract: This paper describes the search of new, high-inclination clusters in the main belt asteroid population, using the D-criterion. Introduction Thanks to the availability of Synthetic proper elements (Knezevic and Milani, 2000) it was possible to apply the D-criterion (Lindblad and Southworth, 1994) to find new clusters in the highly inclined main belt asteroid population. www.uai.it /sez_ast/family/index.htm

SPACE.com -- More Asteroids in Main Belt, New Infrared Survey Says Asteroids in the main belt are not generally considered to be a threat to Earth anytime in the near future, so the new estimate is not likely to alter calculations of the risk of our planet being hit by one. Based on observations of portions of the main asteroid belt, between Mars and Jupiter, the new study estimates there are between 1.1 million and 1.9 million of these large space rocks. But Tedesco and Desert said that improved knowledge of the number and size distribution of asteroids in the main belt is essential to understand the population of NEAs, since most are believed to be former main belt asteroids. www.space.com /scienceastronomy/solarsystem/more_asteroids_020405.html

THE PRIMORDIAL EXCITATION AND DEPLETION OF THE MAIN BELT THE PRIMORDIAL EXCITATION AND DEPLETION OF THE MAIN BELT The asteroid belt is characterized by a large dynamical excitation, an important mass depletion compared to its original density, and a radial mixing of bodies with different physical/chemical properties. Although both approaches are fairly good at structuring the asteroid belt and depleting it, it is likely that both mechanisms occurred at one time or another. www.obs-besancon.fr /publi/petit/Preprints/Excit2.html

Spider-Man's Equipment Belt Spider-Man's web cartridge belt is made out of brass and light leather and holds up to 30 cartridges. The cartridges are presurized to 300 pounds per square inch and sealed with a bronze cap which is silver soldered closed. www.spidey-net.com /main/suit/belt.shtml

The main belt as source of Near-Earth Asteroids The component of the NEA population with dynamical lifetimes shorter than or of the order of 1 Myr can vary by a factor reaching up to a few tens, due to single large-scale collisions in the main belt; these fluctuations are enhanced for smaller bodies and faster evolutionary time scales. We investigate the flux of main-belt asteroid fragments into resonant orbits converting them into near-Earth asteroids (NEAs), and the variability of this flux due to chance interasteroidal collisions. The assumed main-belt asteroid size distribution is derived from that of known asteroids extrapolated down to sizes of ~40 cm, modified in such a way to yield a quasi-stationary fragment production rate over times ~ 100 Myr. earn.dlr.de /abstract/aa4.htm

Main Asteroid Belt The Main Asteroid Belt is only a small remnant of the material that once resided in the region between Mars and Jupiter, but once may have contained between two to 10 Earth masses of material (Dan Durda, "Ask Astro," Astronomy, December 2000). Although no asteroid in the Main Belt grew big enough to hold on to an atmosphere, minerals found in some meteorites suggest that liquid water was often present. It has been estimated that the total mass of the Main Asteroid Belt may total less than 1/1000th of the mass of the Earth. www.solstation.com /stars/asteroid.htm

lec14.html Note that the main belt asteroids are close enough to the Sun to have been boiled dry if they ever contained gases or low boiling point ices! Asteroids are mostly found in a belt of orbits, mostly confined to a narrow range of orbits. They have eccentric orbits and the ones we see, in the inner solar system, seem to be the ones deflected from their original orbits either in the Kuiper belt just outside the orbit of Pluto, or from the Oort cloud in the outskirts of the solar system. www.astro.psu.edu /users/steinn/Astro1/lec14.html

A survey of the dynamics of main belt asteroids II In the outer main belt the asteroids suffer from very strong perturbations in model I and model II, which may throw most of the asteroids out of that region. From our results we can conclude that the main features of the inner part of of the belt (up to the 2:1 resonance) change according to the presence of secular resonances in the new model. We present the second part of a survey of the dynamical structure of the asteroid belt. www.astro.univie.ac.at /~dvorak/publications/abs/9502.html

Synthetic Proper Elements for Outer Main Belt Asteroids (ResearchIndex) Abstract: For the orbits with low to moderate inclination and eccentricity, in the asteroid main belt, the analytically computed proper elements are accurate to a level very close to the best result achievable by any analytical theory. Synthetic Proper Elements for Outer Main Belt Asteroids Synthetic Proper Elements for Outer Main Belt Asteroids (ResearchIndex) citeseer.ist.psu.edu /375569.html

What is the squealing noise coming from the main belt-engine area in a '99 Cavalier that gets louder as the car accelerates? This is not for following-up or discussing "What is the squealing noise coming from the main belt-engine area in a '99 Cavalier that gets louder as the car accelerates?" FAQ Farm only allows simple questions and answers. Contribute a new answer to "What is the squealing noise coming from the main belt-engine area in a '99 Cavalier that gets louder as the car accelerates?" Check the tensioner and make sure it has the correct tension on the serpentine belt. www.faqfarm.com /Car/Repair/61442

belt_bulletin_main Belt Is Spanked Down Under Impact At Loading Point Allowing Material To Be Trapped Under Skirts. Belt Moves Sideways, After Making A Complete Revalution, And Generally Moves A Constant Distance Off Of Center. All Portions of The Conveyor Belt Run To One Side At A Given Point On The Structure. www.blairrubber.com /lining_bulletin_detail.php?id=17

A Closer Look at Main-Belt Asteroids 1: WF/PC Images The probability of four cosmic ray hits of the same profile, brightness, and position with respect to the main asteroid (who’s position on the chip changed due to the different wedge of the different filters) is vanishingly small. While the companions of 45 Eugenia and 107 Camilla are noticeably redder than the main body in the visible region, the companion of 87 Sylvia has substantially the same color. Images in the right column are stretched to have –10 DN be black, and +20 DN to be white, save for the last which is stretched between –10 and +100 DN. www.towson.edu /~astorrs/research/cpaper.htm

StarDate Online Solar System Guide Asteroids Billions of years ago, when the planets were forming, many large asteroids may have inhabited the asteroid belt. Still, the mass of all the asteroids combined is less than the mass of the smallest planet, Pluto. Asteroids are made mostly of rock, often rich in iron and other metals, and perhaps some ice. stardate.org /resources/ssguide/asteroids.html

Main Belt Asteroids Region B is taken to be the collection of main belt asteroids (0.01 deg / hour is ~0.6 arcsec / minute, consistent with the main belt). The plots below show data on Main Belt Asteroids, based on KBO search observations by David Jewitt taken at CFHT with the CFH12K Feb, 1999. Region A is taken to represent the false positive detection rate. panstarrs.ifa.hawaii.edu /project/people/magnier/rocks

Asteroid Introduction Most, however, are contained within a main belt that exists between the orbits of Mars and Jupiter. Spacecraft that have flown through the asteroid belt have found that the belt is really quite empty and that asteroids are separated by very large distances. Some have orbits that cross Earth's path and some have even hit the Earth in times past. www.solarviews.com /eng/asteroid.htm

(9453) 1998 FO1 It is a fairly typical Main Belt asteroid, although with a semi-major axis somewhat larger than average and hence an orbital period significantly longer than that of asteroids such as Ceres, or Vesta. Gareth Williams has calculated the following orbit for (9453) 1998 FO1, which was published in Minor Planet Circular 32642. www.iac.es /galeria/mrk/9453.html

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