Evidence for a Black Hole in the X-Ray Transient GRS 1009–45

1998/12/01 by Aya Kubota, Yasuo Tanaka, Kazuo Makishima +5 · 333 citations
Decision Sciences · Engineering · Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Compact star #Mechanics and Biomechanics Studies #Neutron star #Nova (rocket) #Optics #Photon #Physics #Scientific Measurement and Uncertainty Evaluation

paper · pdf · doi:10.1093/pasj/50.6.667

published in Publications of the Astronomical Society of Japan 50(6), 667-673 (Oxford University Press)

openalex publication_date 1998/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06

Abstract

We report on the result of an X-ray observation of the X-ray Nova Velorum 1993 (GRS 1009–45), made with ASCA on 1993 November 10-11. The energy spectrum was extremely soft and accompanied by a hard tail, characteristics of the Galactic black-hole binaries in the soft state. It is well represented by a two-component model consisting of a multicolor disk model or a general relativistic accretion disk model, both describing emission from an optically thick accretion disk, and a power-law component with a photon index of ∼ 2.5. A spectral analysis of the soft component allows an estimation of the mass of the central object. For the optically-estimated distance (> 1 kpc) and inclination (> 37°), the mass is estimated to be \gt 3.1 M_\odot. These results strongly support that the compact object is a black hole.

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