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Estimation of the spin of a supermassive black hole in Sagittarius A*
- Authors: Andrianov A.S.1, Chernov S.V.1
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Affiliations:
- Lebedev Physical Institute
- Issue: Vol 101, No 3 (2024)
- Pages: 208-212
- Section: Articles
- URL: https://rjmseer.com/0004-6299/article/view/647597
- DOI: https://doi.org/10.31857/S0004629924030017
- EDN: https://elibrary.ru/KKBQQJ
- ID: 647597
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Abstract
In April 2017, the Event Horizon telescope received an image of a supermassive black hole in the Sagittarius A* source. This image consists of a ring-like structure that contains three areas with increased brightness (spots). If we assume that these spots are associated with flares near the event horizon of a black hole, then we can estimate its spin. Our estimate gives a value of the order of a ≈ 0.9.
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About the authors
A. S. Andrianov
Lebedev Physical Institute
Author for correspondence.
Email: andrian@asc.rssi.ru
Astro Space Center
Russian Federation, MoscowS. V. Chernov
Lebedev Physical Institute
Email: chernov@td.lpi.ru
Astro Space Center
Russian Federation, MoscowReferences
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Supplementary files
Supplementary Files
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1.
JATS XML
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Fig. 1. Flash in the accretion disc of the SMBH and its reflection in the first three photon rings
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Fig. 2. The reconstructed VLBI image of a prolonged flare in the accretion disc and its reflection in the first two photon rings, taking into account the constraints of the ngEHT VLBI network
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Fig. 3. Image of the SMBH in Sagittarius A* observed by TGS [1]. Straight lines connect the positions of flares in the disc in both the first and second photon rings, forming an angle that depends only on the spin of the black hole
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5.
Fig. 4. Dependence of the angle between the positions of flares in the disc and in photon rings on the spin of the black hole. The blue line shows the theoretical dependence. The red line shows the dependence calculated taking into account the error in determining the positions of the bright spots in the VLBI images. The error is determined by the limited filling of the spatial frequency region in real VLBI observations
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