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LONG FADING MID-INFRARED EMISSION IN TRANSIENT CORONAL LINE EMITTERS: DUST ECHO OF A TIDAL DISRUPTION FLARE
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationLONG FADING MID-INFRARED EMISSION IN TRANSIENT CORONAL LINE EMITTERS: DUST ECHO OF A TIDAL DISRUPTION FLARE 2016, 832 (2):188 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractThe sporadic accretion following the tidal disruption of a star by a super-massive black hole (TDE) leads to a bright. UV and soft X-ray flare in the galactic nucleus. The gas and dust surrounding the black hole responses to such a flare with an echo in emission lines and infrared emission. In this paper, we report the detection of long fading mid-IR emission lasting up to 14 years after the flare in four TDE candidates with transient coronal lines using the WISE public data release. We estimate that the reprocessed mid-IR luminosities are in the range between 4 x 10(42) and 2 x 10(43) erg s(-1) and dust temperature in the range of 570-800 K when WISE first detected these sources three to five years after the flare. Both luminosity and dust temperature decrease with time. We interpret the mid-IR emission as the infrared echo of the tidal disruption flare. We estimate the UV luminosity at the peak flare to be 1 to 30 times 10(44) erg s(-1) and that for. warm dust masses to be. in the range of 0.05-1.3 M-circle dot within a few parsecs. Our results suggest that the. mid-infrared echo is a general signature of TDE in the gas-rich environment.
VersionFinal published version
SponsorsNational Basic Research Program of China [2015CB857005]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; NSFC [NSFC-11233002, NSFC-11421303, U1431229]; CAS [U1431229]; Fundamental Research Funds for the Central Universities; CAS "Light of West China" Program [2015-XBQN-B-5]; National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration