The disk-bearing young star IM Lupi: X-ray properties and limits on accretion

Article


Gunther, H. M., Matt, S. P., Schmitt, J. H. M. M., Gudel, M., Li, Z. Y. and Burton, D. M.. 2010. "The disk-bearing young star IM Lupi: X-ray properties and limits on accretion." Astronomy and Astrophysics: a European journal. 519 (10), p. A97. https://doi.org/10.1051/0004-6361/201014386
Article Title

The disk-bearing young star IM Lupi: X-ray properties and limits on accretion

ERA Journal ID1050
Article CategoryArticle
AuthorsGunther, H. M. (Author), Matt, S. P. (Author), Schmitt, J. H. M. M. (Author), Gudel, M. (Author), Li, Z. Y. (Author) and Burton, D. M. (Author)
Journal TitleAstronomy and Astrophysics: a European journal
Journal Citation519 (10), p. A97
Number of Pages10
Year2010
PublisherEDP Sciences
Place of PublicationLes Ulis, France
ISSN0004-6361
1432-0746
Digital Object Identifier (DOI)https://doi.org/10.1051/0004-6361/201014386
Abstract

Context. Classical T Tauri stars (CTTS) differ in their X-ray signatures from older pre-main sequence stars, e.g. weaklined TTS (WTTS). CTTS show a soft excess and deviations from the low-density coronal limit in the He-like triplets.
Aims. We test whether these features correlate with accretion or the presence of a disk by observing IM Lup, a diskbearing object apparently in transition between CTTS and WTTS without obvious accretion.
Methods. We analyse a Chandra grating spectrum and additional XMM-Newton data of IM Lup and accompanying
optical spectra, some of them taken simultaneously to the X-ray observations. We fit the X-ray emission lines and
decompose the H emission line in different components.
Results. In X-rays IM Lup has a bright and hot active corona, where elements of low first-ionisation potential are
depleted. The He-like Ne ix triplet is in the low-density state, but due to the small number of counts a high-density
scenario cannot be excluded on the 90% confidence level. In all X-ray properties IM Lup resembles a main-sequence
star, but it is also compatible with CTTS signatures on the 90% confidence level, thus we cannot decide if the soft
excess and deviations from the low-density coronal limit in the He-like triplets in CTTS require accretion or only the
presence of a disk. IM Lup is chromospherically active, which explains most of the emission in H. Despite its low
equivalent width, the complexity of the H line profile is reminiscent of CTTS. We present an estimate for the mass
accretion rate of 10−11M yr−1.

Keywordsstars; formation; individual; IM Lupi; X-rays
ANZSRC Field of Research 2020510109. Stellar astronomy and planetary systems
519999. Other physical sciences not elsewhere classified
330399. Design not elsewhere classified
Public Notes

© 2010 ESO. Deposited in accordance with the copyright policy of the publisher.

Byline AffiliationsCenter for Astrophysics Harvard and Smithsonian, United States
NASA Ames Research Center, United States
University of Hamburg, Germany
University of Virginia, United States
Faculty of Sciences
Institution of OriginUniversity of Southern Queensland
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