1 / 27

Tidal Disruption Events

Tidal Disruption Events. Andrew Levan University of Warwick. r T = R * (M CO / M * ) 1/3. Bound, falls back. Unbound, escapes. r T = R * (M CO / M * ) 1/3. Bound, falls back. Unbound, escapes. WD, NS, BH. r T = R * (M CO / M * ) 1/3. Bound, falls back. Unbound, escapes.

peterz
Download Presentation

Tidal Disruption Events

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Tidal Disruption Events Andrew Levan University of Warwick

  2. rT =R* (MCO / M*)1/3 Bound, falls back Unbound, escapes

  3. rT =R* (MCO / M*)1/3 Bound, falls back Unbound, escapes WD, NS, BH

  4. rT =R* (MCO / M*)1/3 Bound, falls back Unbound, escapes Asteroid, planet, star (MS, WD, RG, NS) WD, NS, BH

  5. rT =R* (MBH / M*)1/3 Rs ~ 2 GM / c2

  6. rT =R* (MBH / M*)1/3 tmin ~ R*3/2 MBH1/2 Duration of event: WD = hours MS = months - years RG = decades - centuries

  7. Tidal disruption events – around massive black holes Probe of the existence of massive BHs in faint galaxies, even globular clusters? Timescales much more rapid than in AGN to probe accretion physics Contribution to the AGN LF Reverberation mapping of circumnuclear material Signposts of gravitational wave sources Signatures of merging BHs (disruption rates 1 per decade) Possible accelerators of ultra-high energy cosmic rays

  8. Finding TDEs Nuclear X-ray and/or optical flares Hot blackbody components (UV, soft X-ray spectrum) Characteristic decay t-5/3 Rates 10-4-5 /yr/L* galaxy (0.1-1% of core collapse SNe rate)

  9. Except…… Nuclear AGN and multiple variable X-ray sources. Often relatively poor X-ray cadence (don’t realise until it is late) X-ray’s often give poor positions compared to optical/radio Nuclear supernovae more common than TDEs Some UV bright at early times, extinction always a concern. Nuclei are bright, and often excluded from optical transient searches due to difficulties in subtractions Contributions from disc, wind etc complicate the lightcurve.

  10. Early work(X-ray’s) Halpern, Gezari & Komossa 2004 ApJ 604 572 Komossa & Bade 1999 A&A 343 775

  11. Recent work(X-ray’s) Saxton et al. 2012 A&A 541 106

  12. Recent work (optical) Gezari et al. 2012 Nature 485 217 Wavelength (A)

  13. Opt UV Recent work (optical) ASASSN-14ae (200 Mpc) HST (13 June 2014) Holoein et al. 2014 arXiv:1405.1417

  14. PS1-10jh Why not both? NUV X-ray Just disc/wind temperature? Different components at different times? Lodato & Rossi 2011 MNRAS 410 359

  15. ULGRB TDE? LGRB SGRB SGR Galactic Sources Levan et al. 2014 ApJ 781 13

  16. Swift J1644+57 Levan et al. 2011 Science 333 199 Levan et al. 2011 Science 333 199, Bloom et al. 2011 Science 333 202

  17. Levan et al. 2011, Cenko et al. 2012, Brown et al. in prep

  18. In context Levan et al. 2011, Cenko et al. 2012

  19. Host Galaxies Levan et al. 2011 Science 333 199 All 3 events consistent with nuclei of their hosts

  20. Bloom et al 2011 Science 333 202

  21. Swift J1644+57 Relativistic outflow Zauderer et al. 2011 Nature 476 425

  22. Swift J1644+57 Switch-off

  23. Swift J2058+0516 Switch-off

  24. Implications A unique probe of galactic nuclei Miller & Gultekin 2011 ApJ 738 13; Berger et al. 2012 arXiv 1112.1697 Host galaxies with MB <-18 have massive black holes in their cores

  25. Jets are rare 3 relativistic TDEs at z=0.35, 0.89, 1.19 All well detected by Swift No other compelling candidates in BAT archive Jetted TDE rate ~10-6“classical TDEs” Jet angles much larger than this Requirements for jet creation unclear

  26. PS1-10jh D23H-1 D3-13 D1-9 PS1-11af ASASSN-14ae PTF09ge PTF09axc PTF09djl NGC5905 RXJ1242-1119 RXJ1420+5334 NGC3599 SDSSJ1323+4827 TDXFJ1347-3254 SDSSJ1311-0123 2MMMi J1847-6317 SDSSJ1201+3003 Swift J1644+57 Swift J2058+0516 Swift J1112-8238 Ultra-long GRBs? UV/optical X-ray Relativistic PTF10iya Are these all TDEs? Why are they so diverse? A naming convention ala SNe is urgently needed (NT-X 2014A?)

  27. Summary and next steps • TDEs are exceptionally useful astrophysical probes • But: Candidates to date are extremely diverse. • X-ray detected events have poor optical follow-up • Many optically detected events don’t have detectable X-ray’s • Jetted events appear to be extremely rare • We still need to understand the physical mechanisms at play to cleanly identify TDEs from other transients, and deploy them as probes. • Multiwavelength follow-up in close to real time is essential • Rule out SNe • Tie events to SMBH as tightly as possible • Map emission processes

More Related