2008
DOI: 10.1051/0004-6361:200809986
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Abstract: Context. Our Galaxy hosts at its dynamical center Sgr A*, the closest supermassive black hole. Surprisingly, its luminosity is several orders of magnitude lower than the Eddington luminosity. However, the recent observations of occasional rapid X-ray flares from Sgr A* provide constraints on the accretion and radiation mechanisms at work close to its event horizon. Aims. Our aim is to investigate the flaring activity of Sgr A* and to constrain the physical properties of the X-ray flares. Methods. In Spring 200… Show more

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Cited by 126 publications
(237 citation statements)
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“…The X-ray data cover a comparatively large and rather densely sampled spectral range. We get χ 2 red ≤ 2 if the X-ray information is weighted higher by a factor of two or more (see Porquet et al 2008;Dodds-Eden et al 2009). A χ 2 -based comparison of different single component emission models over a large wavelength range (radio or infrared till X-ray) is, however, only of limited value.…”
Section: Discussionmentioning
confidence: 98%
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“…The X-ray data cover a comparatively large and rather densely sampled spectral range. We get χ 2 red ≤ 2 if the X-ray information is weighted higher by a factor of two or more (see Porquet et al 2008;Dodds-Eden et al 2009). A χ 2 -based comparison of different single component emission models over a large wavelength range (radio or infrared till X-ray) is, however, only of limited value.…”
Section: Discussionmentioning
confidence: 98%
“…In Table 1 we list important properties of the three brightest X-ray flares that have been observed to date (Baganoff et al 2001;Porquet et al 2003Porquet et al , 2008. The NIR flare emission shows observed spectral indices of α ∼ 0.6 (Ghez et al 2005a,b;Hornstein et al 2006) or even steeper (Eisenhauer et al 2005;Gillessen et al 2006).…”
Section: Ssc Model Of the Bright Flares Of Sgra*mentioning
confidence: 99%
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“…The compact nature of Sgr A has been demonstrated both by direct VLBI measurements (Shen et al 2005) and by the observation of Xray and near IR flares with timescales as short as a few minutes (see for example Porquet et al 2008;Eckart et al 2006; supported by CAPES Foundation, Ministry of Education of Brazil. Porquet et al 2003).…”
Section: Introductionmentioning
confidence: 99%
“…Variability on these timescales limits the emission region to within <10 Schwarzschild radii (R S ) of the black hole. X-ray flares from Sgr A reach peak luminosities of 4 ×10 35 erg s −1 , two orders of magnitude brighter than the quiescent value (Porquet et al 2003;Baganoff et al 2003), and exhibit a range of spectral shapes (Porquet et al 2008). Several models of the origin of this variable emission exist, many of which invoke non-thermal processes close to the event horizon of the central black hole to produce a population of relativistic particles (see e.g.…”
Section: Introductionmentioning
confidence: 99%