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	T Tauri star - Wikipedia, the free encyclopedia
		T Tauri stars are a class of variable stars named after their prototype - T Tauri.
		T Tauri stars are the youngest visible stars.
		A hypothesised T Tauri stage for our Solar System would be one means by which the angular momentum of the contracting Sun was transferred to the protoplanetary disc and hence, eventually to the planets.
	en.wikipedia.org /wiki/T_Tauri_star (447 words)

	T Tauri - Wikipedia, the free encyclopedia
		T Tauri is a variable star in the constellation Taurus, the prototype of the T Tauri stars.
		The T Tauri system consists of at least three stars, only one of which is visible at optical wavelengths; the other two shine in the infrared and one of them also emits radio waves.
		Through VLA radio observations, it was found that the young star (the "T Tauri star" itself) dramatically changed its orbit after a close encounter with one of its companions and may have been ejected from the system.
	en.wikipedia.org /wiki/T_Tauri (278 words)

	T Tauri star
		T Tauri stars are found only in nebulae or very young clusters, have low-temperature (G to M type) spectra with strong emission lines and broad absorption lines.
		They are more luminous than main sequence stars of similar spectral types, and they have a high lithium abundance, which is a pointer to their extreme youth, as lithium is rapidly destroyed in stellar interiors.
		The weak T Tauri stars are of particular interest since they provide astronomers with a look at early stages of stellar evolution unencumbered by nebulous material.
	www.daviddarling.info /encyclopedia/T/TTauri.html (395 words)

	AAVSO: T Tauri, February 2001 Variable Star Of The Month
		Brightness changes detected in these stars are not due to evolutionary effects, per se, but may be due to such processes as instabilities in the disk, violent activity in the atmosphere of the star, and may also be due in part to moving clouds of dust and gas from which they were conceived.
		He chose T Tauri to be the protoype of the class since "it is best known, is among the brightest, and represents the group with respect to both emission and absorption spectra." Up to this point, these stars had been classified as irregular variables.
		T Tauri stars can further be divided into two types and are based on spectroscopic characteristics that arise from their disk properties: the classic T Tauri and weak T Tauri stars.
	www.aavso.org /vstar/vsots/0201.shtml (2432 words)

	T Tauri
		Not far from T Tauri, Hind found a reflection nebula, now called Hind’s Variable Nebula, illuminated at the whim of its unreliable neighbor.
		Then in 1890, nearly 40 years after the discovery of the strange star, Shelburn Burnham found that T Tauri itself is nestled within a very small nebula, now known popularly as Burnham’s Nebula.
		As if all this were not enough, T Tauri turns out to have a binary companion, detected by its infrared glow, 0.5" to 0.7" to the south (hence known as T Tauri S, while T Tauri becomes T Tauri N), and there is even data to such that T Tauri is a triple-star system.
	www.daviddarling.info /encyclopedia/T/T_Tauri.html (296 words)

	The Distance to a Stellar Youngster by Ken Croswell
		T Tauri is the prototype for a class of newborn stars.
		T Tauri consists of at least three stars, one that shines in visible light and two that glow at infrared wavelengths.
		T Tauri itself is a 10th-magnitude star about 4 degrees northwest of Aldebaran, the brightest star in Taurus.
	kencroswell.com /TTauri.html (649 words)

	2MASS Atlas Image Gallery
		This star is an example of a Herbig Be star, which are the massive pre-stellar equivalents of the lower-mass T Tauri stars.
		Herbig Ae/Be stars are the intermediate-mass (2 to 8 solar masses) counterparts of T Tauri stars.
		The Herbig Ae/Be stars are intermediate-mass pre-main sequence objects, showing emission lines in their optical spectra and appearing with associated nebulosity (they are more massive than their lower-mass counterparts, the T Tauri stars).
	www.ipac.caltech.edu /2mass/gallery/images_ysos.html (3316 words)

	Star Clusters
		Stars lighter than those of spectral types O and B are also formed from the same cloud of gas, and reside in the same region of space.
		The formation of low-mass stars like the Sun can be explained by the gravitational collapse of a molecular cloud fragment into a protostellar core and the subsequent accretion of gas and dust from the surrounding interstellar medium.
		Stars in these clusters that are 600 million years old are just now exhausting their central hydrogen fuel, indicating that M82 brightening occurred just that long ago.
	universe-review.ca /F06-star-cluster.htm (2480 words)

	Vanderbilt University Daily Register
		Young stars similar to the sun that are less than 10 billion years old are called T Tauri stars, and they come in two types.
		Classical T Tauri stars are covered in dense clouds of gas and dust and have exceptionally bright “hydrogen alpha” emission lines that are given off by heated hydrogen gas.
		However, comparison of observations taken in December 2004 and April 2005 indicate that the classical T Tauri star was five times brighter in December than it was in the spring, indicating that this star was flaring during the first observation period.
	www.vanderbilt.edu /register/articles?id=20156 (802 words)

	What's Up - Featured Deep Sky Objects (Jan-Feb)
		We now know better; the star, T Tauri, is shrouded in dark dust clouds, and these are indeed moving around, but the much larger nebula NGC 1555 is merely lit up by T Tauri - what we are seeing is a giant shadow show across a vast curtain of gases.
		As T Tauri's dust bubble writhes and shifts, different portions of the neighboring nebula are illuminated.
		T Tauri is interesting in that its odd light variations - subtle changes, from magnitude 9 to 13 - betray a star in its infancy, recently formed from the dark dust in the area.
	www.sciencecenter.net /whatsup/02/ngc1555.htm (262 words)

	[No title] (Site not responding. Last check: 2007-10-08)
		One consequence of this collapse is that young stars (T Tauri stars) are usually surrounded by massive, opaque, circumstellar disks.
		Somehow a fraction of the material accreted onto the star is ejected perpendicular to the disk plane in a highly collimated stellar jet.
		Young stars also have dark spots on their surfaces which are analogous to sunspots but cover a much larger fraction of the surface area of the star.
	sparky.rice.edu /~hartigan/images/slides/sl1.html (149 words)

	THE INFRARED UNIVERSE - Star Formation
		Stars form from collapsing clouds of gas and dust.
		As the cloud collapses, its density and temperature increase.
		Infrared studies of star forming regions will give us important information about how stars are born and thus on how our own Sun and Solar System were formed.
	www.ipac.caltech.edu /Outreach/Edu/sform.html (673 words)

	Search Results for "T Tauri Star"
		...Aldebaran is a visual binary star and an irregular variable star, with magnitude ranging from 0.78 to 0.93.
		It consists of about 100 stars all moving in the same direction.
		Its shape is that of an oblate spheroid, with...
	www.bartleby.com /cgi-bin/texis/webinator/65search?query=T+Tauri+Star (170 words)

	Eric E Mamajek: Annual Report 2002
		The unique stellar sample is in the important age range of ~10-20 Myr, when solar-type stars are contracting on their radiative tracks and supposed to be spinning up due to conservation of angular momentum.
		Mamajek investigated the kinematics of the T Tauri star population of the MBM 12 molecular cloud.
		Using the Gould Belt velocity field as a kinematic model, the proper motions of the MBM 12 T Tauri stars are consistent with the far distance estimates (~300 pc).
	www.as.arizona.edu /Astro/steward/annrep02/Eric_Mamajek.html (662 words)

	T Tauri star concept from the Astronomy knowledge base
		They are believed to be still in the process of gravitational contraction from their protostellar phase and have not yet arrived at the main sequence and begun to burn hydrogen.
		has definition Also called T Tauri variable, a type of variable star of spectral classification F, G or K (giants above the main sequence on the Hertzsprung-Russell diagram) that loses an appreciable proportion of its mass in its (irregular) more luminous periods, and is thus surrounded by volumes of gas and dust.
		YY Orionis star (1 kind, 6 facts) - Very young, late-type, low-mass stars in the gravitationally contracting stage in which the star is still accreting matter from the protostellar cloud.
	www.site.uottawa.ca:4321 /astronomy/TTauristar.html (522 words)

	Sz 68 (Site not responding. Last check: 2007-10-08)
		Sz 68 is a relatively early type T Tauri star, K2IV, hence the star itself is intrinsically bright.
		Sz 68 is often classified as a weak T Tauri star because the H-alpha equivalent width is relatively low, but Sz 68 is an actively accreting T Tauri star with a close circumstellar disk.
		The image of this star is also dominated by a large starspot; however, this time the spot is not centered on the rotation pole, but sits near a latitude of 45 degrees.
	sprg.ssl.berkeley.edu /~cmj/html/sz68.html (576 words)

	APOD Search Results for "T Tauri stars"
		Explanation: A mere 168,000 light-years distant, this large, lovely cluster of stars, NGC 1850, is located near the outskirts of the central bar structure in our neighboring galaxy, the Large Magellanic Cloud.
		NGC 1850 is also a double star cluster, with a second, compact cluster of stars visible here below and to the right of the large cluster's central region.
		Stars in the large cluster are estimated to be 50 million years young, while stars in the compact cluster are younger still, with an age of about 4 million years.
	antwrp.gsfc.nasa.gov /cgi-bin/apod/apod_search?T+Tauri+stars (490 words)

	General Information (Site not responding. Last check: 2007-10-08)
		High resolution spectropolarimetry of the classical T Tauri star T Tau is presented.
		The star was observed in McDonald observatory in southeast Texas.
		For verification, longitudinal magnetic fields for the asteroid Vesta (Sun) and the magnetic Ap star 53 cam were also calculated and agree well with previously published results.
	www.ruf.rice.edu /~agdaou/index_files/Page1349.htm (85 words)

	[No title] (Site not responding. Last check: 2007-10-08)
		The star is known for its unusually high and variable nonthermal radio continuum emission.
		Optically, the spectrum exhibits rather weak characteristics of `classical' T Tauri stars.
		Five models for the magnetic geometry around the star are discussed; solar-type activity, dipole magnetosphere, star-disk magnetic coupling, disk magnetic fields, and close binary interaction.
	www.lowell.edu /users/jch/sss/res/db/pubs/199403.txt (186 words)

	T Tauri Stars (Site not responding. Last check: 2007-10-08)
		As the forming stars slowly contract trying to reach densities and temperatures in their cores which are high enough to ignite fusion, an interesting thing happens to low mass clouds.
		Further, we know that the number of stars for a given mass is larger the smaller the mass of the star, e.g., M stars are much more common than O stars.
		Surprisingly, there appears to be a gap between the lowest mass stars and brown dwarfs and planets in terms of mass.
	zebu.uoregon.edu /~imamura/208/feb15/tauri.html (712 words)

	Periodicities in T Tauri Star Line Profiles (Site not responding. Last check: 2007-10-08)
		As of the writing of this abstract, 3 of 6 stars show evidence for periodic behavior in some portion of their line profiles.
		The remaining 2 stars with detected periods in their line profile variations (DF Tau and DR Tau) do not match known photometric periods.
		The stars which have not shown periodic profile variations so far are RW Aur, RY Tau, and T Tau.
	www.aas.org /publications/baas/v25n4/aas183/abs/S4006.html (204 words)

	APOD: 2001 June 4 - The T Tauri Star Forming System (Site not responding. Last check: 2007-10-08)
		T Tauri system, one of the brighter star systems toward the
		T Tauri system itself, which turns out to be a binary.
		At that time, a new star will shine.
	antwrp.gsfc.nasa.gov /apod/ap010604.html (192 words)

	T Tauri star Comparison Table
		A kind of T Tau stars with considerable changes in brightness.
		A T Tauri star with a strong ultraviolet excess.
		Very young, late-type, low-mass stars in the gravitationally contracting stage in which the star is still accreting matter from the protostellar cloud.
	www.site.uottawa.ca:4321 /astronomy/TTauristar_table.html (121 words)

	[No title]
		The photometric variability and rotational evolution of T Tauri stars.
		Multisite UBVRI photometry of 24 pre-main-sequence stars of the Taurus-Auriga cloud Astron.
		311, 748 (2000) * T.Hearty, R.Neuhaeuser, B.Stelzer, M.Fernandez, J.M.Alcala, E.Covino, V.Hambaryan ROSAT PSPC observations of T Tauri stars in MBM 12 Astron.
	www.iaa.es /~matilde/curringles (2414 words)

	The T Tauri star population in the Lupus star forming region
		The T Tauri star population in the Lupus star forming region
		We estimate effective temperatures and luminosities for the stars observed, and derive masses and ages by comparison with theoretical evolutionary tracks.
		The mean age of WTTS seen in projection against the dark clouds is found to be lower than the mean age of WTTS discovered far from regions of high obscuration, and yet higher than the mean age of the classical T Tauri stars (CTTS) in Lupus.
	www.cs.wisc.edu /niagara/data/nasa/A+A_320_185.xml (242 words)

	[60.15] The Environment and Outflow of the G-type T Tauri Star SU Aur (Site not responding. Last check: 2007-10-08)
		The STIS data demonstrate that this nebulosity consists of a fan of nebulosity similar to that seen around R CrA, with wisp and clump structure down to the resolution limit of the telescope.
		The STIS data demonstrate that this feature is accompanied, on the opposite side of the star, by a string of bow-shaped nebulosities, extending 7.3" (1100 AU) from the star at PA=114+/-1 degrees.
		Given the small number of coronagraphically imaged intermediate-mass stars, this result indicates that collimated outflows, similar to those routinely detected in association with lower mass T Tauri stars, appear to be common among their higher mass analogs and to persist for much of the star's pre-main sequence lifetime.
	www.aas.org /publications/baas/v33n4/aas199/568.htm (479 words)

	Encyclopedia Galactica - Ta to Td - Human (Anglic) Revised 351st Edition
		T-Groups work to coordinate and organize the mental and physical resources of their members to accelerate the process of mental and physical enhancement that can eventually lead to transcension to a higher level.
		They constitute a type of variable star, often shedding mass, still forming and contracting; and yet to evolve to reach the main sequence.
		T Tauri stars are mostly between 105 and 108 years in age; of low mass (0.5 to 3.0 Msol); surrounded by hot, dense envelopes; and losing mass via
	www.orionsarm.com /eg/t/Ta-Td.html (1967 words)

	Astronomy 250: Syllabus
		Emission from T Tauri Stars," Astrophysical Journal, 586, 1136-1147.
		Weintraub, D.A., Kastner, J.H., Bary, J. 2000, "Detection of Quiescent Molecular Hydrogen Gas in the Circumstellar Disk of a Classical T Tauri Star," Astrophysical Journal, 541, 767-771.
		Weintraub, D.A., Sandell, G., Huard, T.L., Kastner, J.H., van den Ancker, M.E., and Waters, R. 1999, "Submillimeter Imaging of T Tauri's Circumbinary Disk and the Discovery of a Protostar in Hind's Nebula," Astrophysical Journal, 517, 819-828.
	www.vanderbilt.edu /AnS/physics/cv/weintraub_cv/papers.htm (1327 words)

	TiO Photometry of Naked T Tauri Stars: V410 Tau
		Modeling of the light curves and Doppler imaging techniques indicate the light variations primarily arise from the rotational modulation by large dark starspot regions, distributed unevenly over its surface.
		This TiO-index, when calibrated with Wing standard stars, yielded a measure of the strength of the TiO absorption band at 719 nm relative to a continuum region at 754 nm.
		for cool stars and is also present in cooler sunspot and starspot regions.
	www.astronomy.villanova.edu /OBS_REPORT/ObsRept2003/node12.html (309 words)

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