Stable and unstable accretion in the classical T Tauri stars IM Lup and RU Lup as observed by MOST. Issue 4 (13th January 2016)

• Record Type: Journal Article
• Authors: Siwak, Michal; Ogloza, Waldemar; Rucinski, Slavek M.; Moffat, Anthony F. J.; Matthews, Jaymie M.; Cameron, Chris; Guenther, David B.; Kuschnig, Rainer; Rowe, Jason F.; Sasselov, Dimitar; Weiss, Werner W.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 456:Issue 4(2016)
• Page Start: 3972
• Page End: 3984
• Publication Date: 2016-01-13
• Subjects: accretion, accretion discs -- stars: individual: RU Lup -- stars: individual: IM Lup -- stars: rotation -- stars: variables: T Tauri, Herbig Ae/Be; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stv2848
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: Results of the time variability monitoring of the two classical T Tauri stars, RU Lup and IM Lup, are presented. Three photometric data sets were utilized: (1) simultaneous (same field) MOST satellite observations over four weeks in each of the years 2012 and 2013, (2) multicolour observations at the South African Astronomical Observatory in April–May of 2013, (3) archival V -filter All Sky Automated Survey (ASAS) data for nine seasons, 2001–2009. They were augmented by an analysis of high-resolution, public-domain VLT-UT2 Ultraviolet Visual Echelle Spectrograph spectra from the years 2000 to 2012. From the MOST observations, we infer that irregular light variations of RU Lup are caused by stochastic variability of hotspots induced by unstable accretion. In contrast, the MOST light curves of IM Lup are fairly regular and modulated with a period of about 7.19–7.58 d, which is in accord with ASAS observations showing a well-defined 7.247 ± 0.026 d periodicity. We propose that this is the rotational period of IM Lup and is due to the changing visibility of two antipodal hotspots created near the stellar magnetic poles during the stable process of accretion. Re-analysis of RU Lup high-resolution spectra with the broadening function approach reveals signs of a large polar coldspot, which is fairly stable over 13 years. As the star rotates, the spot-induced depression of intensity in the broadening function profiles changes cyclically with period 3.710 58 d, which was previously found by the spectral cross-correlation method.