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Radio Properties of Tidal Disruption Events

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Abstract

Radio observations of tidal disruption events (TDEs) probe material ejected by the disruption of stars by supermassive black holes (SMBHs), uniquely tracing the formation and evolution of jets and outflows, revealing details of the disruption hydrodynamics, and illuminating the environments around previously-dormant SMBHs. To date, observations reveal a surprisingly diverse population. A small fraction of TDEs (at most a few percent) have been observed to produce radio-luminous mildly relativistic jets. The remainder of the population are radio quiet, producing less luminous jets, non-relativistic outflows or, possibly, no radio emission at all. Here, we review the radio observations that have been made of TDEs to date and discuss possible explanations for their properties, focusing on detected sources and, in particular, on the two best-studied events: Sw J1644+57 and ASASSN-14li. We also discuss what we have learned about the host galaxies of TDEs from radio observations and review constraints on the rates of bright and faint radio outflows in TDEs. Upcoming X-ray, optical, near-IR, and radio surveys will greatly expand the sample of TDEs, and technological advances open the exciting possibility of discovering a sample of TDEs in the radio band unbiased by host galaxy extinction.

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Notes

  1. We make several simplifying assumptions, most importantly that the magnetic field is constant over the emitting region, and that all electrons are accelerated into a single power-law distribution of energies, \(N_{e}(E) \propto E^{-p}\) for \(E > E_{0}\) (\(E_{0}\) is typically taken to be ≳ the electron rest mass energy). This is typically the case for single impulsive events like GRBs and TDE jets, but is not always true. For example, the compact jet cores of AGN typically have flat spectra because we are observing a superposition of many different synchrotron components.

  2. Sw J1644+57 was also observed at 149 MHz by LOFAR, but the resulting non-detection is not constraining (Cendes et al. 2014).

  3. We note that the available observations only sparsely sample Sgr A*’s density profile, so in principle deviations from \(r^{-1}\) over a narrower range of radii could be present.

  4. We note that this result is only valid for models in which the radio emission arises from an external (forward) shock (Sects. 3.2.1 and 3.2.2). In the model presented by Pasham and van Velzen (2018) (Sect. 3.2.3), the radio emission arises internal to the jet and thus does not provide any information about the density profile of the external medium. However, because the data prefer a freely-expanding jet, Pasham and van Velzen (2018) infer that the external density must be low.

  5. assuming all TDEs that launch radio-loud jets also produce bright \(\gamma \)-ray emission when viewed on-axis.

  6. A more complete list of radio transient surveys and additional details can be found at http://www.tauceti.caltech.edu/kunal/radio-transient-surveys/index.html.

  7. https://astronomers.skatelescope.org.

  8. While the ngVLA has a much smaller field of view than the SKA under the current design, its exquisite sensitivity at high frequencies will make it a key tool for the follow up and discovery of TDEs. Additionally, its milliarcsecond resolution will be very interesting for VLBI observations of nearby events (van Velzen et al. 2018).

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Acknowledgements

We acknowledge useful discussions with the attendees of the ISSI TDE workshop in October 2018, in particular Tsvi Piran. KDA acknowledges support provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51403.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. BAZ acknowledges support while serving at the National Science Foundation (NSF) and from the Dark Cosmology Centre (DARK) at the University of Copenhagen. Any opinion, findings, and conclusions expressed in this material are those of the authors and do not necessarily reflect the views of the supporting agencies.

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Authors and Affiliations

  1. Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL, 60208, USA

    Kate D. Alexander

  2. Center for Cosmology and Particle Physics, New York University, New York, NY, 10003, USA

    Sjoert van Velzen

  3. The Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, 91904, Israel

    Assaf Horesh

  4. Division of Astronomical Sciences, National Science Foundation, 2415 Eisenhower Ave., Alexandria, VA, 22314, USA

    B. Ashley Zauderer

  5. Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100, Copenhagen, Denmark

    B. Ashley Zauderer

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  1. Kate D. Alexander
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  2. Sjoert van Velzen
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  3. Assaf Horesh
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  4. B. Ashley Zauderer
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Correspondence to Kate D. Alexander.

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The Tidal Disruption of Stars by Massive Black Holes

Edited by Peter G. Jonker, Sterl Phinney, Elena Maria Rossi, Sjoert van Velzen, Iair Arcavi and Maurizio Falanga

Kate D. Alexander is NASA Einstein Fellow.

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Alexander, K.D., van Velzen, S., Horesh, A. et al. Radio Properties of Tidal Disruption Events. Space Sci Rev 216, 81 (2020). https://doi.org/10.1007/s11214-020-00702-w

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