Photometric variability of TW Hya from seconds to years as seen from space and the ground during 2013–2017. Issue 1 (2nd June 2018)

• Record Type: Journal Article
• Authors: Siwak, Michal; Ogloza, Waldemar; Moffat, Anthony F J; Matthews, Jaymie M; Rucinski, Slavek M; Kallinger, Thomas; Kuschnig, Rainer; Cameron, Chris; Weiss, Werner W; Rowe, Jason F; Guenther, David B; Sasselov, Dimitar
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 478:Issue 1(2018)
• Page Start: 758
• Page End: 783
• Publication Date: 2018-06-02
• Subjects: stars: individual: TW Hya -- stars: variables: T Tauri, Herbig Ae/Be; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1220
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: This is the final photometric study of TW Hya based on new MOST satellite observations. During 2014 and 2017, the light curves showed stable 3.75- and 3.69-d quasi-periodic oscillations, respectively. Both values appear to be closely related to the stellar rotation period, as they might be created by changing visibility of a hotspot formed near the magnetic pole directed towards the observer. These major light variations were superimposed on a chaotic, flaring-type activity caused by hotspots resulting from unstable accretion – a situation reminiscent of that in 2011, when TW Hya showed signs of a moderately stable accretion state. In 2015, only drifting quasi-periods were observed, similar to those present in 2008–2009 data and typical for magnetized stars accreting in a strongly unstable regime. A rich set of multicolour data was obtained during 2013–2017 with the primary aim of characterizing the basic spectral properties of the mysterious occultations in TW Hya. Although several possible occultation-like events were identified, they are not as well defined as in the 2011 MOST data. The new ground-based and MOST data show a dozen previously unnoticed flares, as well as small-amplitude 11 min–3 h brightness variations, associated with 'accretion bursts'. We cannot exclude the possibility that the shortest 11–15 min variations could also be caused by thermal instability oscillations in an accretion shock.