GRO J1655−40 is a binary star consisting of an evolved F-type primary star and a massive, unseen companion, which orbit each other once every 2.6 days in the constellation of Scorpius. Gas from the surface of the visible star is accreted onto the dark companion, which appears to be a stellar black hole with several times the mass of the Sun. GRO J1655-40 is an X-ray nova black-hole-candidate binary discovered during an outburst in 1994. Its orbital period has been measured in the visible as 2.62 days, and it exhibits irregular outburst activity. Dynamical measurements suggest that the compact object is a ~7 solar mass black hole.
GRO J165540 moving through the Milky Way, illustration Stock Image C056/6049 Science
the observational data in GRO J1655-40, we apply a variety of twin HF QPO models based on the frequencies of the geodesic epicyclic motion of matter in accretion discs orbiting Kerr black holes, i.e. the orbital (azimuthal) frequency of the circular mo- tion, or the radial and vertical epicyclic frequencies. The analysis of the disk wind of GRO J1655-40, or J1655 for short, confirmed what astronomers had long suspected, namely that magnetic friction is central to understanding how black holes accrete matter rapidly. Without a process to take away some of the angular momentum of the gas, it could remain in orbit around a black hole for a very long time. GRO J1655-40: Evidence for a Spinning Black Hole Drawing Credit: A. Hobart, CXC Explanation: In the center of a swirling whirlpool of hot gas is likely a beast that has never been seen directly: a black hole. We report photometric and spectroscopic observations of the black hole binary GRO J1655-40 in complete quiescence. In contrast to the 1995 photometry, the light curves from 1996 are almost completely dominated by ellipsoidal modulations from the secondary star.
StellarMass Black Holes
GRO J1655-40, a recently discovered black-hole candidate, is an ideal system for studying jets of material from the accretion disk around a black hole. Observations of the radio emission show two. GRO J1655−40 is a well-studied Galactic low-mass X-ray binary (Hjellming & Rupen 1995; Orosz et al. 1997; Abramowicz & Kluźniak 2001), whose distance is d ∼ 3.2 kpc (Hjellming & Rupen 1995), orbital period is 2.6 d (Greene, Bailyn & Orosz 2001), and black hole mass is M BH = 5.4 ± 0.3 M ⊙ while the companion star has mass M s = 1.45 ±. GRO J1655−40 was observed on 20 occasions and data were obtained by all instruments for the majority of epochs. X-ray spectroscopy revealed spectral shapes consistent with the 'canonical' low/hard, high/soft and very high states at various epochs. The soft X-ray source (0.3-10 keV) rose from quiescence and entered the low/hard state. Main. We obtained a high-resolution spectrum of the secondary star in the eclipsing low-mass X-ray binary GRO J1655-40, in quiescence phase, on 24 May 1998 with the 10-m Keck I telescope. This.
(PDF) On the distance of GRO J165540
GRO J1655-40 One of the paradoxes of black holes is that although they are completely dark -- they release no detectable energy of any kind -- they produce some of the brightest and most powerful phenomena in the universe. Many are surrounded by disks of superhot gas known as "accretion disks." GRO J1655-40: Early Stages of the 2005 Outburst - NASA Technical Reports Server (NTRS) As of October 27, 2023, NASA STI Services will no longer have an embargo for accepted manuscripts. For more information visit NTRS News. Back to Results
Artist's View of Black Hole and Companion Star GRO J1655-40. 3224 of 4503. Next. Orbit of Black Hole in the Milky Way Galaxy. About This Image. Release Date November 18, 2002 10:00AM (EST) Read the Release Release ID: 2002-30 Permissions Content Use Policy Download Options. 800 X 600, JPG (27.76 KB) GRO J1655-40: Evidence for a Spinning Black Hole. Drawing Credit: A. Hobart, CXC. Explanation: In the center of a swirling whirlpool of hot gas is likely a beast that has never been seen directly: a black hole. Studies of the bright light emitted by the swirling gas frequently indicate not only that a black hole is present, but also likely.
ESA Closeup of the blackhole system GRO J165540
of GRO J1655−40 during its 2005 outburst rise, which was first detected on February 17 (MJD 53419) with the Propor-tional Counter Array (PCA) instrument on-board the Rossi X-ray Timing Explorer (RXTE) (Markwardt & Swank 2005). The source was intensely monitored with RXTE throughout this outburst. There was also exceptional multi- NASA / ESA Hubble Space Telescope image shows the Year 2001 observation of the black hole system GRO J1655-40 in the constellation of Scorpius. Hubble's high resolution has allowed astronomers to measure the motion of this black-hole system across the sky using this image and an image taken in 1996. Scientists combined the Hubble data with.
