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Topic: Eunomia asteroids

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15 Eunomia

	15 Eunomia - Wikipedia, the free encyclopedia
		It is the largest of the stony (S-type) asteroids, and somewhere between the 8th to 12th largest Main Belt asteroid overall (uncertainty in diameters causes uncertainty in its ranking).
		The range of compositions of the remaining Eunomia family members, formed by a collision of the common parent body, is large enough to encompass all the surface variations on Eunomia itself.
		An older explanation of the compositional differences, that Eunomia is a mantle fragment of a far larger parent body (with a bit of crust on one end, and a bit of core on the other) appears to be ruled out by studies of the mass distribution of the entire Eunomia family of asteroids.
	en.wikipedia.org /wiki/15_Eunomia (829 words)

	asteroid
		Most asteroids move in orbits that are somewhat more inclined and eccentric than those of the major planets (with the exception of Pluto) – the orbit of an average main-belt asteroid being inclined at about 10° to the plane of the ecliptic with an eccentricity of about 0.15.
		Following its discovery, an asteroid is given a preliminary designation that consists of the year of discovery, an upper case letter to indicate the half-month in that year (A=Jan 1-15, B=Jan 16-31,..., Y=Dec 16-31, the letter “I” being omitted), and a second upper case letter in sequence.
		The distribution of the various classes throughout the asteroid belt is highly structured, suggesting that many asteroids formed at or near their present distances from the Sun and are representative of the composition of the solar nebula (not including hydrogen and helium) at these locations.
	www.daviddarling.info /encyclopedia/A/asteroid.html (1793 words)

	Minor planet (Site not responding. Last check: 2007-10-24)
		Nysa asteroids have a mean orbital radius between 2.41 AU and 2.5 AU, an eccentricity between 0.12 and 0.21, and an inclination between 1.5° and 4.3°.
		Alinda asteroids have a mean orbital radius of 2.5 AU and an eccentricity between 0.4 and 0.65 (approximately).
		Eos asteroids have a mean orbital radius between 2.99 AU and 3.03 AU, an eccentricity between 0.01 and 0.13, and an inclination between 8° and 12°.
	www.aseannewsnetwork.de /articles/content/m/mi/minor_planet.html (2088 words)

	Asteroids (Site not responding. Last check: 2007-10-24)
		Asteroids are primoridal objects left over from the formation of the Solar System (see schematic diagram of nomenclature and relationships among asteroids, Edgeworth-Kuiper bodies, and comets and their different subgroups by William K. Hartmann).
		Indeed, if all asteroids down to the size of meter- or yard-sized boulders or less were combined together, the resulting object would measure less than 1,300 to 1,500 km (810 to 930 miles) across, which is less than one third to one half the diameter of the Earth's Moon.
		Smaller asteroids, however, should be solid bodies because the shattered fragments of an asteroidal collision should easily escape their feeble gravity and fly off into space instead of settling back on their surface as regolith.
	www.wingmakers.co.nz /Asteroids.html (1474 words)

	2 The asteroid masses and densities
		In the case of lack of additional perturbing asteroids in the extended dynamical models, the masses for the standard model were retained and used for calculation of the weighted mean of the mass.
		Asteroid masses in these models are taken from Table 6 and one should realize that they can be erroneous.
		For the latter two asteroids the differences between their masses for the standard and the extended dynamical models are much larger and reach about 100% and 200%, respectively, in comparison to the masses for the standard model.
	aanda.u-strasbg.fr:2002 /papers/aa/full/2001/29/aa10228/node2.html (4009 words)

	search.com - Minor planet
		Eos asteroids have a semi-major axis between 2.99 AU and 3.03 AU, an eccentricity between 0.01 and 0.13, and an inclination between 8° and 12°.
		Nysa asteroids have a semi-major axis between 2.41 AU and 2.5 AU, an eccentricity between 0.12 and 0.21, and an inclination between 1.5° and 4.3°.
		Maria asteroids have a semi-major axis between 2.5 AU and 2.706 AU and an inclination between 12° and 17°.
	domainhelp.search.com /reference/Minor_planet (2397 words)

	Asteroid Introduction
		Asteroids are rocky and metallic objects that orbit the Sun but are too small to be considered planets.
		Asteroids that are on a collision course with Earth are called meteoroids.
		Then on October 1991 asteroid 951 Gaspra was visited by the Galileo spacecraft and became the first asteroid to have hi-resolution images taken of it.
	www.solarviews.com /eng/asteroid.htm (543 words)

	Asteroids
		Asteroids are classified into a number of types according to their spectra (and hence their chemical composition) and albedo:
		Between the main concentrations of asteroids in the Main Belt are relatively empty regions known as the Kirkwood gaps.
		It is a particularly interesting asteroid in that it seems to have been differentiated into layers like the terrestrial planets.
	www.seds.org /nineplanets/nineplanets/asteroids.html (1354 words)

	Yarkovsky Effect and the Dynamics of the Solar System (Site not responding. Last check: 2007-10-24)
		For the S-type families (Flora, Maria, Eos, Eunomia and Koronis) we assumed a low-conductive regolith of the thermal conductivity K=0.001 W/m/K (the thermal capacity is 680 J/kg/K and the surface density is 1.5 g/cm^3).
		In the low-inclination ``frames'' we may notice a ``jet'' of asteroids with low values of proper(a) and proper(e), a structure that may be formed by the resonance.
		You see, that the result is not ``that excellent as before'', since the frequent reorientations of small-size asteroids prevent them to diffuse due to Yarkovsky orbital effect very far from their initial positions (hence the ``bell-shaped'' distribution of the final semimajor axes in the 1-5 km size bin).
	sirrah.troja.mff.cuni.cz /~mira/mp/Yarko_fam/dora_eos_themis.html (8363 words)

	Astronomy Course Notes
		Asteroids are named with (i) a number indicating the order of discovery, starting from 1, and (ii) a proper name sometimes suggested by the discoverer.
		Asteroids are composed of rock, which distinguishes them from comets; the latter have a high proportion of low-density, icy material that is emitted when they are warmed by the Sun.
		Asteroids are too small for radioactive heating to have made them molten, unlike the terrestrial planets.
	astro.wsu.edu /allen/courses/notes/asteroids.html (1412 words)

	Asteroid (15) Eunomia in 2006 (Site not responding. Last check: 2007-10-24)
		The asteroid is at its first stationary point on June 10 when its westerly motion commences, the second is on September 17 when it returns to moving in a prograde sense towards the east.
		Eunomia's orbital period is 4.30 years, its distance from the Sun varying between 2.15 and 3.14 AU, with an eccentricity of.186.
		The orbit is inclined at 11.750° to the ecliptic.
	www.rasnz.org.nz /MinorP/Eunomia.htm (432 words)

	Ephemerides of the Largest Asteroids
		However, because the asteroids have relatively little mass and are subject to perturbations by other asteroids the actual uncertainties in their mean motions are likely to be a few tenths of an arcsecond per century.
		Asteroid perturbations are the largest source of incompletely modeled perturbations of the planets especially Mars and the Earth-Moon barycenter.
		The perturbing asteroids included in the ephemeris of each asteroid are given in Table 4.The mass for Interamnia was the mean of two values determined by Landgraff (1992).
	aa.usno.navy.mil /hilton/ephemerides/asteroid_ephemerides.html (9264 words)

	Masses of the Largest Asteroids
		The perturbation of asteroids on Mars and the Earth are the largest poorly modeled problem in modern planetary ephemerides.
		The asteroids were not always considered to be a type of body separate from those of the other planets.
		Hilton, J.L. 1997, The Mass of the Asteroid 15 Eunomia From Observations of 1313 Berna and 1284 Latvia, Astron.
	www.pinecity.k12.mn.us /highschool/Astronomy/masses_asteroids.htm (1082 words)

	A/CC Catalog: Asteroids 1-499 (Site not responding. Last check: 2007-10-24)
		Ceres is the largest of the Main Belt asteroids in mass and diameter, with a width exceeding 900 km.
		This was the second asteroid binary discovered, and the first to be resolved as separate objects by Earth-based observations (from the Canada-France-Hawaii Telescope in infrared using adaptive optics).
		It is an S-type Main Belt asteroid with a diameter estimated at 67.6 km.
	www.hohmanntransfer.com /cat/an1.htm (1707 words)

	Resorting Query Results
		We describe the creation of a model of the main asteroid belt whose purpose is to describe the main-belt asteroid size frequency distribution and simulate the number of main-belt asteroids and their fluxes at visual through mid-infrared (~0.3-70 μm) wavelengths in any area of sky for an arbitrary date.
		asteroids obtained from the complete known asteroid sample, plus extrapolation of the size-frequency distributions of 15 asteroid dynamical families and three background populations, to a diameter limit of 1 km.
		, 1973, Icarus 19, 507 522; Gaffey and McCord, 1979, Mineralogical and petrological characterizations of asteroids.
	www-ssg.sr.unh.edu /IAU_Comm15/Archives/WGMP_2005_Refs.htm (3742 words)

	Asteroid models
		Asteroids and comets form the largest and, perhaps paradoxically, the least well known population of celestial bodies in our solar system.
		Especially binary asteroids (both contact and separate, and both near-Earth and main-belt asteroids) are currently an area of very active research.
		A recent example of this was the first analysis of an asteroid family thought to have been formed in a catastrophic collision.
	www.rni.helsinki.fi /~mjk/asteroids.html (1143 words)

	[No title]
		We will study it with the FOC F/288 high resolution mode line_7: to determine the absolute diameter (and thus calibrate the asteroid diameter line_8: scales), the irregularities of the body, and the reasons for variations during line_9: its rotation (about 9.1 hours).
		line_15: Several asteroids are suspected to consist not only of one single body, but to line_16: be binary or multiple in nature, or to have satellites.
		The scheduling of the line_2: observations is therefore closely tied to the ST launch date and to the line_3: availability of the moving target acquisition mode.
	ecf.hq.eso.org /poa/FOS/props/3346c.prop (1307 words)

	ASTEROIDS (Site not responding. Last check: 2007-10-24)
		Over 3,300 major asteroids are numbered, but hundreds of thousands smaller ones may exist.
		The second and third characters "W7" are a shorthand way of counting the number of asteroids found during the 2nd half of August 2000.
		The first asteroid discovered was "2000 QA"; the second was "2000 QB;" The second letter cycles through the alphabet until it reaches "Z" and then it goes back to the beginning with an extra number.
	www.il-st-acad-sci.org /planets/asteroid.html (255 words)

	Main-Belt asteroids (Site not responding. Last check: 2007-10-24)
		The aim of the project is to independently determine the orbits of several (at least 4) asteroids by making a series of positional measurements.
		This is achieved by measuring the asteroid's position on a CCD image relative to that of catalogued stars.
		The position of the asteroid is measured relative to the catalogued stars.
	www.dur.ac.uk /john.lucey/astrolab/mainbelt.html (372 words)

	The Night Sky This Week
		Asteroids, also called minor planets, are rocky bodies that orbit the Sun within our solar system.
		Asteroid 6 Hebe, named after the Greek goddess of youth, cupbearer for the gods of Mount Olympus, looks like an ordinary field star glowing at magnitude 7.9.
		A month ago, the Lincoln Laboratory Near-Earth Asteroid Research robotic telescope detected an object which was reported as a minor planet of magnitude 17.1, and after careful orbit calculations it was obvious that this was Barnard's lost comet.
	www.nightskyinfo.com (2229 words)

	Asteroids Section Current Events (Site not responding. Last check: 2007-10-24)
		The asteroid Herculina, 207 kilometers in diameter, will be brighter than magnitude 10 and visible in the constellations Serpens and Ophiuchus from late April to late July, 2006.
		The asteroid Hebe, 190 kilometers in diameter, will be brighter than magnitude 10 and visible in the constellations Aquarius, and Capricornus from mid May to early November, 2006.
		The asteroid Eunomia, 320 kilometers in diameter, will be brighter than magnitude 10 and visible in the constellations Capricornus, Aquarius, and Sagittarius from late May to mid October, 2006.
	www.rasc.ca /observing/asteroids/astevents.html (663 words)

	Asteroids (Site not responding. Last check: 2007-10-24)
		They are portrayed in their correct relative sizes and shapes (the limb of Mars is shown for comparison); colors and albedos are also indicated.
		The following graph shows the number density of asteroids as a funciton of their distance from the sun.
		These asteroids are located approximately at the leading and trailing Lagrangian (i.e.
	alumnus.caltech.edu /~marcsulf/asteroid/asteroid.html (445 words)

	15 Eunomia
		It was discovered by A. de Gasparis on July 29, 1851 and named after Eunomia, one of the Horae (Hours), a personification of order and law in Greek mythology.
		Eunomia has rather variable lightcurve indicating an elongated object.
		This led to a suggestion that Eunomia may be a binary object.
	www.mlahanas.de /Greeks/Astro/15Eunomia.html (181 words)

	[No title]
		Astronomers pay careful attention to the Near Earth Asteroids due to their importance roule in the Earth's neighbourhood; other asteroids do not get the same attention, and if they were not be observed for a longer time, they are considered as lost.
		During the past century the Trojan asteroids were the topic of many studies of their orbital dynamics and stability.
		An observing methodology has been developed whereby the asteroid is imaged using an unfiltered 0.28-m aperture Schmidt-Cass telescope having a field of view of 11'x8' whilst simultaneous V- and I-band images are obtained of a wider 1.0x1.5 degree field using two 0.06-m refractors equipped with CCD cameras.
	www.astrometrica.at /MACE/abstracts.html (3760 words)

	References on Asteroid Masses (Site not responding. Last check: 2007-10-24)
		This set of references, to the best of my knowledge, is a complete list of all scientific sources in which the mass of one or more asteroids is determined.
		Bange, J. 1998, "An Estimation of the Mass of Asteroid 20 Massalia Derived from the Hipparcos Minor Planet Data", Astron.
		Scholl, H., Schmadel, L.D., & Roser, 1987, "The Mass of the Asteroid (10) Hygiea Derived from Observations of (829) Academia", Astron.
	aa.usno.navy.mil /hilton/MassReferences.html (813 words)

	Astron. Astrophys. 354, 315-320 (2000) (Site not responding. Last check: 2007-10-24)
		Speckle interferometry measurements of the asteroids 10-Hygiea and 15-Eunomia
		Speckle interferometry measurements of the asteroids 10-Hygiea and 15-Eunomia have been obtained with the speckle facility aboard the AdOpt@TNG module, permanently mounted on the 3.58m TNG telescope in Canary Islands.
		Direct angular diameter measurements and estimates of the apparent ellipticity are given allowing to derive the density of these asteroids, combining our data with published results.
	aa.springer.de /bibs/0354001/2300315/small.htm (141 words)

	Asteroid (6) Hebe (Site not responding. Last check: 2007-10-24)
		It reaches a stationary point on June 25, after which the asteroid will start moving in a westerly, retrograde sense, through the stars as seen from the Earth.
		Three of the brighter asteroids reach opposition during July and August with (15) Eunomia on July 29, Hebe on August 4 and (1) Ceres on August 16.
		The orbit is inclined at 14.8° to the ecliptic.
	www.rasnz.org.nz /MinorP/Hebe.htm (421 words)

	A/CC Catalog Index
		This catalog of asteroid and comet links was the beginning of a much larger site feature now inaugurated as the A/CC Catchall Catalog of Minor Objects.
		Asteroids by [_number__name__designation_] – Comets by [_name__number__designation_] – [top]
		This list consists of asteroids that are unnumbered, or are numbered but not yet named.
	www.hohmanntransfer.com /catchall.htm (178 words)

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