Sub-relativistic Outflow and Hours-Timescale Large-amplitude X-ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
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2024
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| author | Yao, Yuhan Guolo, Muryel Tombesi, Francesco Li, Ruancun Gezari, Suvi García, Javier A. Dai, Lixin Chornock, Ryan Lu, Wenbin Kulkarni, S. R. Gendreau, Keith C. Pasham, Dheeraj R. Cenko, S. Bradley Kara, Erin Margutti, Raffaella Ajay, Yukta Wevers, Thomas Kwan, Tom M. Andreoni, Igor Bloom, Joshua S. Drake, Andrew J. Graham, Matthew J. Hammerstein, Erica Laher, Russ R. LeBaron, Natalie Mahabal, Ashish A. O'Connor, Brendan Purdum, Josiah Ravi, Vikram Sears, Huei Sharma, Yashvi Smith, Roger Sollerman, Jesper Somalwar, Jean J. Wold, Avery |
| author_facet | Yao, Yuhan Guolo, Muryel Tombesi, Francesco Li, Ruancun Gezari, Suvi García, Javier A. Dai, Lixin Chornock, Ryan Lu, Wenbin Kulkarni, S. R. Gendreau, Keith C. Pasham, Dheeraj R. Cenko, S. Bradley Kara, Erin Margutti, Raffaella Ajay, Yukta Wevers, Thomas Kwan, Tom M. Andreoni, Igor Bloom, Joshua S. Drake, Andrew J. Graham, Matthew J. Hammerstein, Erica Laher, Russ R. LeBaron, Natalie Mahabal, Ashish A. O'Connor, Brendan Purdum, Josiah Ravi, Vikram Sears, Huei Sharma, Yashvi Smith, Roger Sollerman, Jesper Somalwar, Jean J. Wold, Avery |
| contents | We present the tidal disruption event (TDE) AT2022lri, hosted in a nearby ($\approx\!144$ Mpc) quiescent galaxy with a low-mass massive black hole ($10^4\,M_\odot < M_{\rm BH} < 10^6\,M_\odot$). AT2022lri belongs to the TDE-H+He subtype. More than 1 Ms of X-ray data were collected with NICER, Swift, and XMM-Newton from 187 d to 672 d after peak. The X-ray luminosity gradually declined from $1.5\times 10^{44}\,{\rm erg\,s^{-1}}$ to $1.5\times 10^{43}\,{\rm erg\,s^{-1}}$ and remains much above the UV and optical luminosity, consistent with a super-Eddington accretion flow viewed face-on. Sporadic strong X-ray dips atop a long-term decline are observed, with variability timescale of $\approx\!0.5$ hr--1 d and amplitude of $\approx\!2$--8. When fitted with simple continuum models, the X-ray spectrum is dominated by a thermal disk component with inner temperature going from $\sim\! 146$ eV to $\sim\! 86$ eV. However, there are residual features that peak around 1 keV, which, in some cases, cannot be reproduced by a single broad emission line. We analyzed a subset of time-resolved spectra with two physically motivated models describing either a scenario where ionized absorbers contribute extra absorption and emission lines or where disk reflection plays an important role. Both models provide good and statistically comparable fits, show that the X-ray dips are correlated with drops in the inner disk temperature, and require the existence of sub-relativistic (0.1--0.3$c$) ionized outflows. We propose that the disk temperature fluctuation stems from episodic drops of the mass accretion rate triggered by magnetic instabilities or/and wobbling of the inner accretion disk along the black hole's spin axis. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_11343 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Sub-relativistic Outflow and Hours-Timescale Large-amplitude X-ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri Yao, Yuhan Guolo, Muryel Tombesi, Francesco Li, Ruancun Gezari, Suvi García, Javier A. Dai, Lixin Chornock, Ryan Lu, Wenbin Kulkarni, S. R. Gendreau, Keith C. Pasham, Dheeraj R. Cenko, S. Bradley Kara, Erin Margutti, Raffaella Ajay, Yukta Wevers, Thomas Kwan, Tom M. Andreoni, Igor Bloom, Joshua S. Drake, Andrew J. Graham, Matthew J. Hammerstein, Erica Laher, Russ R. LeBaron, Natalie Mahabal, Ashish A. O'Connor, Brendan Purdum, Josiah Ravi, Vikram Sears, Huei Sharma, Yashvi Smith, Roger Sollerman, Jesper Somalwar, Jean J. Wold, Avery High Energy Astrophysical Phenomena We present the tidal disruption event (TDE) AT2022lri, hosted in a nearby ($\approx\!144$ Mpc) quiescent galaxy with a low-mass massive black hole ($10^4\,M_\odot < M_{\rm BH} < 10^6\,M_\odot$). AT2022lri belongs to the TDE-H+He subtype. More than 1 Ms of X-ray data were collected with NICER, Swift, and XMM-Newton from 187 d to 672 d after peak. The X-ray luminosity gradually declined from $1.5\times 10^{44}\,{\rm erg\,s^{-1}}$ to $1.5\times 10^{43}\,{\rm erg\,s^{-1}}$ and remains much above the UV and optical luminosity, consistent with a super-Eddington accretion flow viewed face-on. Sporadic strong X-ray dips atop a long-term decline are observed, with variability timescale of $\approx\!0.5$ hr--1 d and amplitude of $\approx\!2$--8. When fitted with simple continuum models, the X-ray spectrum is dominated by a thermal disk component with inner temperature going from $\sim\! 146$ eV to $\sim\! 86$ eV. However, there are residual features that peak around 1 keV, which, in some cases, cannot be reproduced by a single broad emission line. We analyzed a subset of time-resolved spectra with two physically motivated models describing either a scenario where ionized absorbers contribute extra absorption and emission lines or where disk reflection plays an important role. Both models provide good and statistically comparable fits, show that the X-ray dips are correlated with drops in the inner disk temperature, and require the existence of sub-relativistic (0.1--0.3$c$) ionized outflows. We propose that the disk temperature fluctuation stems from episodic drops of the mass accretion rate triggered by magnetic instabilities or/and wobbling of the inner accretion disk along the black hole's spin axis. |
| title | Sub-relativistic Outflow and Hours-Timescale Large-amplitude X-ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2405.11343 |