Delayed X-Ray Brightening Accompanied by Variable Ionized Absorption Following a Tidal Disruption Event

被引:4
|
作者
Wevers, T. [1 ,2 ]
Guolo, M. [3 ]
Pasham, D. R. [4 ]
Coughlin, E. R. [5 ]
Tombesi, F. [6 ,7 ,8 ,9 ,10 ]
Yao, Y. [11 ]
Gezari, S. [1 ,3 ]
机构
[1] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[2] European Southern Observ, Alonso Cordova 3107, Santiago, Chile
[3] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA
[4] Kavli Inst Astrophys & Space Res, MIT, Cambridge, MA 02139 USA
[5] Syracuse Univ, Dept Phys, Syracuse, NY 13210 USA
[6] Tor Vergata Univ Rome, Phys Dept, Via Ric Sci 1, I-00133 Rome, Italy
[7] Via Frascati 33, I-00040 Monte Porzio Catone, Italy
[8] INFN Rome Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy
[9] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[10] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA
[11] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA
来源
ASTROPHYSICAL JOURNAL | 2024年 / 963卷 / 01期
基金
美国国家科学基金会;
关键词
BLACK-HOLE MASSES; SUPER-EDDINGTON ACCRETION; RELATIVISTIC OUTFLOWS; ULTRAFAST OUTFLOW; DISK ACCRETION; FALLBACK RATES; STELLAR; EVOLUTION; MODEL; LINE;
D O I
10.3847/1538-4357/ad1878
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Supermassive black holes can experience super-Eddington peak mass fallback rates following the tidal disruption of a star. The theoretical expectation is that part of the infalling material is expelled by means of an accretion disk wind, whose observational signature includes blueshifted absorption lines of highly ionized species in X-ray spectra. To date, however, only one such ultrafast outflow (UFO) has been reported in the tidal disruption event (TDE) ASASSN-14li. Here we report on the discovery of a transient absorption-like signature in X-ray spectra of the TDE AT2020ksf/Gaia20cjk (at a redshift of z = 0.092), following an X-ray brightening similar to 230 days after UV/optical peak. We find that while no statistically significant absorption features are present initially, they appear on a timescale of several days and remain detected up to 770 days after peak. Simple thermal continuum models, combined with a power-law or neutral absorber, do not describe these features well. Adding a partial-covering, low-velocity ionized absorber improves the fit at early times but fails at late times. A high-velocity (v w similar to 42,000 km s-1), ionized absorber (UFO) provides a good fit to all data. The few-day timescale of variability is consistent with expectations for a clumpy wind. We discuss several scenarios that could explain the X-ray delay, as well as the potential for larger-scale wind feedback. The serendipitous nature of the discovery could suggest a high incidence of UFOs in TDEs, alleviating some of the tension with theoretical expectations.
引用
收藏
页数:17
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