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Topic: Alinda asteroids

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	Alinda family - Encyclopedia, History, Geography and Biography
		The Alinda asteroids are a group of asteroids with a semi-major axis of about 2.5 AU and an orbital eccentricity approximately between 0.4 and 0.65.
		One consequence of this is that if an Alinda asteroid happens to be in an unfavorable position for viewing at the time of its close approach to Earth (for instance, at a small elongation from the Sun), then this situation can persist for decades.
		Indeed, as of 2004, the Alinda asteroids 3360 Syrinx and 1915 Quetzálcoatl had not been observed since 1985, and 2608 Seneca had not been observed since 1994.
	www.arikah.com /encyclopedia/Alinda_asteroid (302 words)

	Alinda group (of asteroids)
		A group of asteroids with a mean orbital radius of about 2.5 AU and an orbital eccentricity between about 0.4 and 0.65.
		One consequence of this is that if an Alinda asteroid happens to be in an unfavorable position for viewing at the time of its close approach to Earth (for instance, at a small elongation from the Sun), then this situation may persist for decades.
		As of 2004, for example, the Alinda asteroids 1981 VA and (1915) Quetzalcoatl had not been observed since 1985, and (2608) Seneca had not been observed since 1994.
	www.daviddarling.info /encyclopedia/A/Alinda_group.html (218 words)

	[No title]
		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°.
		Alinda asteroids have a mean orbital radius of 2.5 AU and an eccentricity between 0.4 and 0.65 (approximately).
	www.thrushobservatory.org /minor/what_are.htm (2129 words)

	Minor planet - Space Wiki - a Wikia wiki (Site not responding. Last check: 2007-10-26)
		Arjuna asteroids are somewhat vaguely defined as having orbits similar to Earth's; ie, with an average orbital radius of around 1 AU and with low eccentricity and inclination.
		Alinda asteroids have a mean orbital radius of 2.5 AU and an eccentricity between 0.4 and 0.65 (approximately).
		Pallas family asteroids have a mean orbital radius between 2.7 and 2.8 AU and an inclination between 30° and 38°.
	space.wikia.com /wiki/Minor_planets (2334 words)

	IV-3
		The distribution of known asteroids as a function of distance from the Sun (semimajor axis a) is shown in figure 1.
		Between 1.8 and 3.5 AU (asteroid belt), this distribution is probably a reasonable representation of the actual distribution, subject to corrections for observational bias against the more distant and lower albedo (fainter) objects in the outer asteroid belt (ref.
		The major difficulty for an asteroidal source for meteorites (and Apollo asteroids) is to modify the orbit from that of a main-belt object to an Earth-approching object in as short a time as indicated by the cosmic-ray exposure age of the meteorites, or at a rate sufficient to maintain the Apollo population.
	www.nas.nasa.gov /About/Education/SpaceSettlement/spaceres/IV-3.html (6466 words)

	Alinda asteroid
		The Alinda asteroids are a group of asteroids with a meanorbital radius of about 2.5 AU and an orbital eccentricity approximately between 0.4 and 0.65.
		One consequence of this is that if an Alinda asteroid happens to be in an unfavorable position for viewing at the time of itsclose approach to Earth (for instance, at a small elongation from the Sun), then thissituation can persist for decades.
		Indeed, as of 2004, the Alinda asteroids 1981 VA and 1915 Quetzalcoatl had not beenobserved since 1985, and 2608 Seneca had not been observed since 1994.
	www.therfcc.org /alinda-asteroid-194266.html (196 words)

	Minor planet at AllExperts
		Sir William Herschel (discoverer of Uranus), coined the term asteroid for the first objects discovered in the 19th century, all of which orbit the sun between Mars and Jupiter, and generally in relatively low-eccentricity (i.e., not very elongated) orbits.
		The overwhelming majority of known asteroids have orbits lying between the orbits of Mars and Jupiter, roughly between 2 to 4 AU.
		* Alinda asteroids have a mean orbital radius of 2.5 AU and an eccentricity between 0.4 and 0.65 (approximately).
	en.allexperts.com /e/m/mi/minor_planet.htm (2331 words)

	Alinda family at AllExperts
		The Alinda asteroids are a group of asteroids with a semi-major axis of about 2.5 AU and an orbital eccentricity approximately between 0.4 and 0.65.
		One consequence of this is that if an Alinda asteroid happens to be in an unfavorable position for viewing at the time of its close approach to Earth (for instance, at a small elongation from the Sun), then this situation can persist for decades.
		Indeed, as of 2004, the Alinda asteroids (3360) 1981 VA and 1915 QuetzÃ¡lcoatl had not been observed since 1985, and 2608 Seneca had not been observed since 1994.
	en.allexperts.com /e/a/al/alinda_family.htm (297 words)

	Resonance - Part 1 of 5
		Based on 87 asteroid orbits, his results were published briefly in 1867 and more fully in 1868, when he listed 97 asteroids ranging from Flora at 2.20 AU to Sylvia at 3.49 AU.
		Asteroids were first found at resonant positions in the following years: 1875: Hilda at 3/2 - 1888: Thule at 4/3 - 1908: Achilles at 1/1 - 1918: Alinda at 3/1 - 1918: Griqua at 2/1.
		In the late 19th century, for example, Simon Newcomb used perturbations in the orbit of the asteroid Polyhymnia to find the mass of Jupiter to be 1/1047.35 that of the sun.
	www7.pair.com /arthur/meteor/archive/archive7/May99/msg00046.html (687 words)

	Asteroids - their history
		The gaps and clusters of asteroids correspond to resonances with Jupiter.
		Asteroids which may cross the Earth's orbit,(and therefore might at some time impact the Earth, with devastating consequences if they are large bodies), are classified into four groups.
		Asteroids with orbits which come closer to the sun than the Earth, are called Atens, and are given ancient Egyptian names.
	homepage.ntlworld.com /heather.hobden1/asteroids.htm (6883 words)

	Minor planet (Site not responding. Last check: 2007-10-26)
		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°.
		Themis asteroids have a semi-major axis between 3.08 AU and 3.24 AU, an eccentricity between 0.09 and 0.22, and an inclination less than 3°.
		A large number of asteroids have orbits between the orbits of Mars and Jupiter, roughly 2 to 4 AU, in a region known as the Main belt.
	minor-planet.iqnaut.net (2279 words)

	Max Wolf - Biocrawler (Site not responding. Last check: 2007-10-26)
		He pioneered the use of astrophotographic techniques to automate the discovery of asteroids, as opposed to older visual methods, as a result of which asteroid discovery rates sharply increased.
		Among his many discoveries was 588 Achilles (the first Trojan asteroid) in 1906, as well as two other Trojans: 659 Nestor and 884 Priamus.
		He also discovered 887 Alinda in 1918, which is now recognized as an Earth-crossing Amor asteroid (or sometimes classified as the namesake of its own Alinda family).
	www.biocrawler.com /encyclopedia/Max_Wolf (338 words)

	Is the Solar System Stable?
		The asteroid's orbit will be considerably affected by Jupiter if conjunctions occur when the asteroid is at its furthermost point from the Sun (aphelion) is where the two orbits are closest.
		The asteroid reaches the danger point of aphelion after three and nine years,but in each case Jupiter is a different point in its orbit.
		At least two asteroids in the gap, Alinda and Quetzalcoatl, are actually in resonance with Jupiter, and 1989 AC, the asteroid that will pass within just 0.011 astronomical units of the Earth in 2004, is also probably in resonance with Jupiter at the gap.
	www.fortunecity.com /emachines/e11/86/solarsys.html (3438 words)

	Utilising an Asteroid to establish a large off-Earth colony in orbit - Abdul Ahad
		An asteroid rich in its surface mineral composition would be economically attractive, since these objects are thought to contain 'rare Earth' metals such as Platinum, Iridium, Rubidium, etc. as part of a mining attraction for the initial orbital venture post orbit capture around the Earth.
		By first establishing a robotic outpost on the candidate asteroid, then through a progressive excavation program utilising robots that dig their way into the body, the end result would be a hollowed out asteroid that provides thousands of square metres of habitat space suitable for housing a moderate sized colony.
		For a brief overview illustration of the astrodynamics requirements, I will choose near Earth asteroid 887 Alinda which is thought to be just 4 km across (2.5 miles), and approaches the orbit of the Earth to within 0.14 AU (20 million km) at perihelion.
	www.astroscience.org /abdul-ahad/earth-ring.htm (2898 words)

	Terraformers Society of Canada - Arjunas (Near Earth Asteroids) (Site not responding. Last check: 2007-10-26)
		Because their eccentricities are very large, about a third of Amor III asteroids have orbits that stretch beyond the asteroid belt and come within 1 au of Jupiter.
		For instance, the first Alinda asteroid (in 1:3 resonance with Jupiter and 4:1 resonance with Earth) discovered was 887 Alinda.
		It is 1-2 km in diameter and is a V-type asteroid, meaning that it may be a fragment of the asteroid 4 Vesta.
	society.terraformers.ca /content/view/44/94/1/4 (1522 words)

	BBC - Astronomy: Stardate
		Toutatis is both an Apollo Asteroid and an Alinda Asteroid.
		Apollo asteroids have mean average distances from the Sun of more than 1 AU (the average Earth-Sun distance - find out how to measure the AU).
		Alinda asteroids have eccentric orbits with average distances from the Sun of 2.5 AU.
	www.open2.net /astronomy/asteroids/toutatis.html (364 words)

	Problems
		The asteroids are a group of small rocky bodies orbiting the sun in relatively circular orbits.
		The vast majority of asteroids lie in the region between the orbits of mars and jupiter known as the main asteroid belt.
		These orbits are empty because they share a simple harmonic relationship with the orbit of jupiter; that is, the ratio of the period of an unoccupied or under-occupied orbit in a Kirkwood gap forms a simple whole number ratio with the period of an orbit of jupiter (something like 2:1 or 3:2 or 5:3).
	hypertextbook.com /physics/mechanics/heliocentrism/problems.shtml (693 words)

	Resonance - Part 4 of 5
		To analyze the properties of asteroids and their orbits, Dermott and Murray defined a parameter d as the measure of the displacement of an asteroid from the nearest strong resonance.
		Thus, they reduced their data set to 144 asteroids, constituting a bias-free set, from which they concluded there is no magnitude-frequency distribution change near the Kirkwood gaps.
		The few asteroids that remain in a libration region tend to have eccentricities much higher than the average of their neighbors.
	www7.pair.com /arthur/meteor/archive/archive7/May99/msg00051.html (624 words)

	IV-1
		Orbital elements of the 53 asteroids with perihelion under 1.5 AU are given in table 1.
		The position of this asteroid is also marked in figure 3, which indicates that the delta-V value to depart from the asteroid to Earth can be as low as 2.3 to 3.4 km/sec (if the relative positions of Earth and the asteroid are those required for the transfer).
		Suppose that delta V at the asteroid is limited to 3 km/sec and the Earth approach speed is limited to the "free" capture speed of 1.5 km/sec.
	www.belmont.k12.ca.us /ralston/programs/itech/SpaceSettlement/spaceres/IV-1.html (4496 words)

	IV-1
		The position of this asteroid is also marked in figure 3, which indicates that the delta-V value to depart from the asteroid to Earth can be as low as 2.3 to 3.4 km/sec (if the relative positions of Earth and the asteroid are those required for the transfer).
		Suppose that delta V at the asteroid is limited to 3 km/sec and the Earth approach speed is limited to the "free" capture speed of 1.5 km/sec.
		Although no satisfactory outbound flight arriving at this asteroid less than 1 year before the return flight was found, it is confidently expected that, as asteroids are studied and more are discovered, cases will be found that do indeed provide retrieval for a total (round-trip) delta V of 5 km/sec.
	www.nss.org /settlement/nasa/spaceres/IV-1.html (4488 words)

	[No title]
		For example, the Trojan asteroids librate (oscillate) around the 1:1 orbital resonance (i.e., the orbital period of Jupiter is in a 1:1 ratio with the orbital period of the Trojan asteroids); the asteroid Thule librates around the 4:3 orbital resonance; and several asteroids in the Hilda group librate around the 3:2 orbital resonance.
		Although the asteroid Griqua librates around the 2:1 resonance with Jupiter, and Alinda librates around the 3:1 resonance, the orbital commensurabilities 2:1, 7:3, 5:2, and 3:1 are characterized by an absence of asteroids in an otherwise rather highly populated, uniform distribution spanning all of the commensurabilities.
		These are the Kirkwood gaps in the distribution of asteroids, and the recent understanding of their creation and maintenance has introduced into celestial mechanics an entirely new concept of irregular, or chaotic, orbits in a system whose equations of motion are entirely deterministic.
	sonic-arts.org /monzo/solarsystem/TD_post_about_calendar.txt (1437 words)

	1862 Apollo Information
		It is the namesake of the Apollo asteroids, and the first one discovered, although because it was lost for a time its asteroid number (1862) is higher than that of some other Apollo asteroids such as 1566 Icarus.
		It was the first asteroid recognized to cross Earth's orbit (although the earlier-discovered 887 Alinda is now known to do so as well).
		On November 4, 2005, it was announced that an asteroid moon, or satellite of Apollo has been detected by radar observations from Arecibo Observatory, Puerto Rico, 29 October–2 November, 2005.
	www.bookrags.com /wiki/1862_Apollo (219 words)

	THE SPACEGUARD DYNAMICAL CLASSIFICATION
		The behavior of the semimajor axis of an Alinda is easily identified, because the resonant perturbations by Jupiter generate large and rapid changes in a, as in the example in Figure 24.
		The problem is, these are the orbits we are not yet able to model analytically in all their complexity, because the combined effects of secular resonances and close approaches to the terrestrial planets play an essential rôle in the evolution of the Oljato class orbits.
		In the near-Earth and near-Mars region other secular resonances, locking the asteroid perihelium and node to the ones of the terrestrial planets, are known to occur [Michel and Froeschlé 1997], [Michel et al.
	copernico.dm.unipi.it /~milani/maratea/node6.html (1209 words)

	The First Nine Clues - Mars-Earth Wars
		The Trojan asteroids are two clumps that have settled in at 300 arc seconds, in 1:1 resonance with Jupiter.
		When asteroids go out of resonance with Jupiter at the 2:1 gap, they go out of resonance by 4%, 5% or 6%.This is their new stability is zone.
		Judging by the paucity of asteroids in the 2:1 resonance, and the numerous asteroids at about 5% one either side, it is judged that the chance that Mars never shifted into a new orbit from a former orbit, since the dawn of history, is estimated at one chance in ten.
	www.creationism.org /patten/PattenMarsEarthWars/PattenMEW11.htm (11036 words)

	ASTEROIDS (Site not responding. Last check: 2007-10-26)
		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)

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