2 edition of X-ray emitting T Tauri stars in the L1551 cloud found in the catalog.
X-ray emitting T Tauri stars in the L1551 cloud
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va
Written in English
|Statement||Lee Carkner ... [et al.].|
|Series||NASA contractor report -- NASA CR-201079.|
|Contributions||Carkner, Lee., United States. National Aeronautics and Space Administration.|
|The Physical Object|
In the case of the visible T Tauri stars, which are sources more evolved than L IRS5, there is evidence 7, 8 that the stars constituting a close binary (that is, a pair with separation of. X-ray Emitting T Tauri Stars in the L Cloud Lee Carkner 1, Eric D. Feigelson, Katsuji Koyama 2, Thierry Montmerle 3, and I. Neill Reid 4 1 Department of Astronomy & Astrophysics, Pennsylvania State University, University Park PA , USA.
The American Astronomical Society (AAS), established in and based in Washington, DC, is the major organization of professional astronomers in North America. Its Cited by: Multiwavelength and Statistical Research in Space Astrophysics Eric D. Feigelson, Principal Investigator of a particularly active star [10, 59], discovered X-ray emitting young stars in distant star forming regions , and clarified the nature of several young stars near the Coalsack . Emitting T Tauri Stars in the L Cloud.
T Tauri stars are pre-main-sequence stars in the process of contracting to the main sequence along the Hayashi track, a luminosity–temperature relationship obeyed by infant stars of less than 3 solar masses (M☉) in the pre-main-sequence phase of stellar evolution. It ends when a star of M☉ develops a radiative zone. that have generated insight into the X-ray emission mechanisms of T Tauri stars. In particular, the density-sensitive line ratios of He-like ions (O vii, Ne ix) detected in the Chandra/HETGS X-ray spectrum of TW Hya indicated plasma densities in the range
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The X-ray luminosity function for the L T Tauri stars is roughly consistent with that found in the Chamaeleon I cloud (FCMG). Most of the detected sources are WTT stars with log L_, No correlation is found between X-ray luminosity and surface rotation velocity, v sin i, for 9 stars with measured rotation.
Low-mass pre-main-sequence stars in the nearby Lynds star-forming cloud are studied with the ROSAT and ASCA X-ray satellites. An 8 ks ROSAT image reveals 38 sources including seven well-known T Tauri stars, two likely new weak-lined T Tauri stars, five potential new weak-lined T Tauri stars, one young B9 star, and the remaining sources are unrelated to.
An 8 ksec ROSAT image reveals 38 sources including X-ray emitting T Tauri stars in the L1551 cloud book well-known T Tauri stars, 14 potential new weak-lined T Tauri stars, 16 X-ray emitting stars unrelated to the cloud, and an active B9 star.
Low mass pre-main sequence stars in the nearby Lynds star forming cloud cloud are studied with the ROSAT and ASCA X-ray satellites.
An 8 ksec ROSAT image reveals 38 sources including 7 well-known T Tauri stars, 14 potential new weak-lined T Tauri stars, 16 X-ray emitting stars unrelated to the cloud, and an active B9 : L.
Carkner, E. Feigelson, K. Koyama, T. Montmerle. Get this from a library. X-ray emitting T Tauri stars in the L cloud. [Lee Carkner; United States. National Aeronautics and Space Administration.;]. Low mass pre-main sequence stars in the nearby Lynds star forming cloud are studied with the ROSAT and ASCA X-ray satellites.
An 8 ksec ROSAT image reveals 38 sources including 7 well-known T Tauri stars, 2 likely new weak-lined T Tauri stars, 5 potential new weak-lined T Tauri stars, one is a young B9 star, and the remaining sources are unrelated to the cloud.
X-ray Emitting T Tauri Stars in the LW Cloud Chapter 4. disruption of the L cloud core can be seen from the sheared clumps and disrupted appearance of the CS emission presented by Moriarty-Schieven et al cluster to form in the L cloud. In Figure 3 we also show contours showing red- and blue-shifted outflowing CO emission.
SAO/NASA Astrophysics Data System (ADS) Title: X-Ray-emitting T Tauri Stars in the L Cloud Authors: Carkner, L., Feigelson, E. D., Koyama, K., Montmerle, T. We present the Chandra ACIS and ASCA GIS results for a series of four long-term observations on D ROXs 21 and ROXs 31; the X-ray brightest T-Tauri stars (TTSs) in the Rho Ophiuchi cloud.
Thomas Preibisch: The origin of X-ray emission from T Tauri stars its. Third, especially in dense clusters, the in-dividual sources could often not be spatially resolved, and so the proper identiﬁcation of the X-ray sources was di cult or impossible.
Finally, in most X-ray data sets, only a rela-tively small number of individual young stars. The L cloud in the Taurus-Auriga complex is one of the best-studied star forming regions at many wavelengths, and was the location where X-ray emitting T Tauri stars were first discovered with the Einstein Observatory.
Our observation with the ROSAT PSPC detector reveal 38 faint soft X-ray sources. They are very rich in magnetically-controlled X-ray phenomena: stellar flares and star-disk interactions in hundreds of T Tauri stars, confined winds in massive stars, : Thomas Preibisch.
1 X-RAY EMISSION FROM CLASSICAL T TAURI STARS J.H.M.M. Schmitt1 1 Hamburger Sternwarte, Universitat¤ g,GojenbergswegD Germany ABSTRACT Young stars produce copious amounts of X-ray emission.
The observedactivity is usually interpretedas a. L cloud in Taurus. X-Ray--emitting T Tauri Stars in the L Cloud Carkner et al. () ApJ28 Orion. New weak-line T Tauri stars in Orion from the ROSAT all-sky survey Alcalá et al. () A&AS7 On the nature of the ROSAT X-ray selected weak-line T Tauri stars in Orion Alcalá et al.
() A&Aobjects (YSOs) in the star-forming complex L in stars present signiﬁcant variability on the ﬁve-day tim e scale. Modulation of the light curve on time scales comparable with the star’s rotational period appeared to be present in the case of one weak-lined T Tauri star.
X-ray emitting T Tauri stars in the L cloud Not In Library. X-ray emitting T Tauri stars in the L cloud Not In Library. X-ray emitting T Tauri stars in the L cloud who have written the most books on this subject.
Lists. watch for edits or export all records. An 8 ksec ROSAT image reveals 38 sources including 7 well-known T Tauri stars, 2 likely new weak-lined T Tauri stars, 5 potential new weak-lined T Tauri stars, one is a young B9 star.
that both coronal magnetic activity and accretion contribute to the observed X-ray emission. We ﬁnd a Ne/O ratio similar to that observed in the much younger classical T Tauri star BP Tau.
From the soft part of the X-ray emission, mostly produced by plasma heated in the accretion shock, we derive a mass accretion rate of 5 ×10−11 M⊙yr−1. T Tauri stars present X-ray luminosities (L X) near the satura-tion limit (log(L X /L bol) = -3) found for main-sequence (MS) stars, L X=L bol ˘10i.e., sometimes orders of magnitude higher than more evolved stars.
For MS stars the X-ray activ-ity is highly related with the rotation period, a relation given by the power law L X/L bol /P Cited by: 4.
Young, low-mass stars are luminous X-ray sources1 whose powerful X-ray flares2,3,4,5,6 may exert a profound influence over the process of planet formation7. The origin of the X-ray emission is Cited by:. This provides the largest X-ray study of a pre-main-sequence stellar population and covers the initial mass function from brown dwarfs up to a 45 M ☉ O star.
Source luminosities span 5 orders of magnitude from log L X to ergs s -1 in the keV band, plasma energies range from to >10 keV, and absorption ranges from log N H. Class II PMS stars also have an accreting disk but the stellar photospheres are now visible in the optical band.
These are the “classical T Tauri stars” discovered decades ago, and the phase can last from ∼ to as long as ∼10 6 years. Class III are the “weak-lined T Tauri stars” where accretion has stopped and the disk is by: 2 Manuel G¤udel et al.: X-rays from jet-driving protostars and T Tauri stars sphere, heating plasma to temperatures of T ˇ3v2 mp=16k ˇ M=R [K] where M and R are the stellar mass and the stellar radius,respectively,in solar units, is themeanmolecular weight, mp is the proton mass, and k is the Boltzmann constant.