IGR J17091-3624

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Double star
IGR J17091-3624
Artist's impression of IGR J17091-3624. A reddish accretion disk can be seen around the black hole, the winds are bluish and emerge above and below the disk. The star from which matter flows into the black hole is shown next to the black hole.
Artist's impression of IGR J17091-3624.

A reddish accretion disk can be seen around the black hole, the winds are bluish and emerge above and below the disk. The star from which matter flows into the black hole is shown next to the black hole.

AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Scorpio
Right ascension 17 h 09 m 0.76 s
declination -36 ° 24 ′ 25.7 ″
Typing
Spectral class F8V + BH
Variable star type LMXB / BHXB / XN + E 
Astrometry
distance 36,000 - 55,000  ly
11,000 - 17,000  pc  
Physical Properties
Dimensions 8.7 - 15.6  M ☉
Other names
and catalog entries
Other names CXOU J170907.6-362425, INTEGRAL1 44, SAX J1709.1-3624, SWIFT J1709.8-3627B, PBC J1709.4-3624, SWIFT J1709.8-3626, KRL2007b 222

IGR J17091-3624 is called L ow M ass X -ray B inary ( LMXB , dt. X-ray binary star systemwith low mass), which consists of a developed star of the spectral class F8 V and a stellar black hole , whichorbiteach other in the constellation Scorpio .

IGR J17091-3624 was discovered by INTEGRAL / IBIS during an observation at the Galactic Center on April 14th and 15th, 2003.

System structure

With its strong gravitational pull, the black hole snatches matter from its companion star (with the designation: 2MASS J17090199-3623260). Due to the conservation of angular momentum, this matter does not fall directly into the black hole, but initially forms a rapidly rotating accretion disk .

A combined mass estimate for the black hole using three different methods gives a mass range of 8.7 to 15.6 M ⊙ with 90% certainty . During an outbreak in 2011, the source developed through intermediate states from the so-called “low / hard state” (LHS) to the “high / soft state” (HSS) spectral state. Using an estimated luminosity at this transition and the simultaneous observations at different frequency ranges, a distance to the solar system of approx. 11 to 17 k pc (approx. 36,000 - 55,000 ly ) was derived for an assumed typical mass of M BH = 10 M ⊙ , which is consistent with the observed radio emissions from the source.

observation

By differential friction in the accretion disk , the gas is heated to millions of degrees, which sends high-energy X-rays , which throughout the galaxy are visible. With changes within the plasma flow in the disk, special X-ray variability patterns occur, which are quasi-periodic outbreaks (English quasi periodic oscillations, QPOs) with frequencies of ≈ 0.1 to 10 Hz , which occur in a period of Repeat for 5 to 70 seconds and pulse like a "heartbeat" with different intensities. A more detailed investigation confirmed the standard hypothesis that the vibrations are due to the limit cycle behavior of an inner disk dominated by unstable radiation pressure . A similar behavior has so far only been observed in the black hole GRS 1915 + 105 , but with outbreaks that are 20 times stronger.

Most of the BHXBs discovered so far are transient X-ray sources that repeatedly show bright bursts. During the beginning of the month-long to year-long outbursts, they go through relatively short-lived intermediate states during the transition from the "low / hard state" (LHS) (with an accretion rate that corresponds to approx. 1% to 10% of the Eddington luminosity ) to the "high / soft state “(HSS) (with an accretion rate of approx. 10% to 50% of the Eddington luminosity). In the “low / hard state” (LHS) the sources typically show hard X-ray spectra .

The standard paradigm for accretion disks in binary systems with black holes is that the inner radius of the disk in the HSS spectral state extends to the innermost stable circular orbit (ISCO), while in the LHS spectral state it is already cut off at a much larger radius becomes. When using relativistic reflection models, it can be seen that the accretion disc is permanently cut off at R in ≥ 10 r g , whereby a slight disc inclination of ≈ 30 ° to 40 ° to the line of sight is assumed.

Spectroscopic investigations of IGR J17091 have clearly shown that accretion disc winds are present in soft, disc-dominated HSS spectral states, and are alternately connected to the stellar jets observed in LHS spectral states.

IGR J17091-3624 blows matter out into space at a speed of 9.3 × 10 3 km s −1 (approx. 0.03 c or 32 million km / h). This could be proven by observations with the Chandra X-ray telescope . It is the highest speed to date for a “disk wind” emanating from a stellar black hole. Up until now, such high speeds were only known from supermassive black holes in galaxy centers . It is believed that the gas flow is driven by strong magnetic fields. Photoionization modeling suggests that this accretion disk wind emanates from the black hole within 43,300 Schwarzschild radii and blows up to 95 percent of the incident matter back out into space.

The term microquasar or Black Hole X-ray Binary (BHXB) is also used in the terminology when the compact component is a black hole.

Together with Cygnus X-1 , GRO J1655-40 and GRS 1915 + 105 , IGR J17091-3624 is one of ten known galactic microquasars (as of 2019).

Web links

Individual evidence

  1. ↑ a b IGR J17091-3624. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed on November 14, 2019 .
  2. ↑ a b I. Negueruela, et al .: A search for counterparts to massive X-ray binaries using photometric catalogs . In: Astronomy & Astrophysics, 461: 631, 2007 . September 29, 2006. arxiv : astro-ph / 0610006 . doi : 10.1051 / 0004-6361: 20066054 .
  3. ↑ a b Rodriguez, et al .: First simultaneous multi-wavelength observations of the black hole candidate IGR J17091−3624 . In: A&A, Volume 533, September 2011 . August 22, 2011. doi : 10.1051 / 0004-6361 / 201117511 .
  4. ^ A b N. Iyer, A. Nandi, S. Mandal: Determination of mass of IGR J17091-3624 from "Spectro-Temporal" variations during onset phase of the 2011 outburst . In: High Energy Astrophysical Phenomena . May 11, 2015. arxiv : 1505.02529 . doi : 10.1088 / 0004-637X / 807/1/108 .
  5. ↑ F. Capitanio, et al .: The peculiar 2011 outburst of the black hole candidate IGR J17091−3624, a GRS 1915 + 105-like source? . In: Monthly Notices of the Royal Astronomical Society, Volume 422, Issue 4, June 2012, Pages 3130-3141, . May 12, 2012. doi : 10.1111 / j.1365-2966.2012.20834.x .
  6. ↑ Mayukh Pahari, et al .: Interpreting the large amplitude X-ray variation of GRS 1915 + 105 and IGR J17091-3624 as modulations of an accretion disc . In: High Energy Astrophysical Phenomena . October 4, 2013. arxiv : 1310.1186 . doi : 10.1093 / mnras / stt1732 .
  7. ↑ Yanjun Xu, et al .: Spectral and Timing Properties of IGR J17091-3624 in the Rising Hard State During its 2016 Outburst . In: High Energy Astrophysical Phenomena . November 13, 2017. arxiv : 1711.04421 . doi : 10.3847 / 1538-4357 / aa9ab4 .
  8. ↑ a b Ashley L. King, et al .: An Extreme X-ray Disk Wind in the Black Hole Candidate IGR J17091-3624 . In: High Energy Astrophysical Phenomena . December 15, 2011. arxiv : 1112.3648 . doi : 10.1088 / 2041-8205 / 746/2 / L20 .
  9. ↑ Mayukh Pahari, et al .: Properties of unique hard X-ray dips observed from GRS 1915 + 105 and IGR J17091-3624 and their implications . In: High Energy Astrophysical Phenomena . September 13, 2013. arxiv : 1309.7213 . doi : 10.1088 / 0004-637X / 778/1/46 .