Rapid infrared flares in GRS 1915+105: evidence for infrared synchrotron emission

Fender, R. P.; Pooley, G. G.; Brocksopp, C.; Newell, S. J.

doi:10.1093/mnras/290.4.l65

Cited by 113 publications

(132 citation statements)

References 16 publications

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“…This result and the derived A K = 3.3 mag (using A v A K from Rieke & Lebofsky 1985) as well, are still used for dereddening (e.g. Fender et al 1997;Fender & Pooley 2000), although the authors pointed out that these results are uncertain (Fender & Pooley 2000). The position of GRS 1915+105 is known very accurately since the discovery of the radio counterpart ).…”

Section: Grs 1915+105 and Its Optical Extinctionmentioning

confidence: 87%

On the optical extinction and distance of GRS 1915+105

Chapuis

Corbel

2004

A&A

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Abstract. Based on new millimeter and radio observations, we reevaluate the total hydrogen column density along the line of sight to the microquasar GRS 1915+105 to N H = (3.5±0.3)×10 22 cm −2 . Our value is consistent with the one derived from X-ray measurements, namely (3.8 ± 0.3) × 10 22 cm −2 (Ebisawa et al. 1998). Using the empirical law between the visual extinction and the total column density of hydrogen, A v is found to 19.6 ± 1.7 mag. This result is ∼7 mag lower than previously thought, and therefore, a reevaluation of infrared fluxes after derredening is needed. The revisited kinematic study allows to give a lower limit to the distance of GRS 1915+105 , namely 6.0 kpc. Taking into account the most accurate upper limit of distance inferred from radio data (11.2 ± 0.8 kpc, Fender et al. 1999) as well as this lower limit, this implies a distance of 9.0 ± 3.0 kpc.

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Section: Grs 1915+105 and Its Optical Extinctionmentioning

confidence: 87%

On the optical extinction and distance of GRS 1915+105

Chapuis

Corbel

2004

A&A

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“…Fender et al (1997) observed rapid flares in the radio and infrared, and found a clear correlation between the two. They interpreted these oscillations as synchrotron emissions from repeated ejection of matter from the system.…”

Section: Introductionmentioning

confidence: 84%

Evidence for local mass accretion rate variations in the disc of GRS 1915+105

Migliari

Belloni²

2003

A&A

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Abstract.We have analysed 16 observations of class β of GRS 1915+105 performed with the Rossi X-ray Timing Explorer. We show the time-resolved evolution (every 16 s) of the X-ray spectral parameters during these observations. The three model independent states (A, B, C) identified in the color-color diagrams are described here in terms of the more physical (and model dependent) quantities of the disc and power law components. As in the color analysis, we observe specific and time-asymmetric transitions between states. Within a single observation, we identified a loop-like cycle of the power law spectral index that starts and ends with the ending of state C. There is evidence of local mass accretion rate variations and mass loss during the long instability intervals (long state C). This is consistent with simultaneous radio and X-ray observations that show a one-to-one relation between the long state C and the radio flares, that occur shortly after it: a loss of disc mass is followed by an ejection of matter in the jet.

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“…GRS 1915ϩ105 exhibits a broad range of correlated multiwavelength variability, including very complex Xray behavior (see, e.g., Muno, Morgan, & Remillard 1999;Markwardt et al 1999;Lin et al 2000), superluminal radio outflows (Mirabel & Rodriguez 1994;Fender & Pooley 2000), and correlated infrared, X-ray, and radio variability (Fender et al 1997;Eikenberry et al 1998;Bandyopadhyay et al 1998). Motivated by the discovery of a second high-frequency QPO in GRO J1655Ϫ40, we analyzed the archival RXTE data from GRS 1915ϩ105 to search for a second QPO in this object as well.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

Strohmayer

2001

The Astrophysical Journal

132

107

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We report the discovery in archival Rossi X-Ray Timing Explorer data of a ∼40 Hz quasi-periodic oscillation (QPO) in the hard X-ray flux from the Galactic microquasar GRS 1915ϩ105. The QPO is detected only in the hard X-ray band above ∼13 keV and was discovered in observations in which the previously known 67 Hz QPO is present. The 40 Hz QPO has a typical rms amplitude of ∼2% in the 13-27 keV band and a width of ∼5.5 Hz (FWHM). We show that the 67 and 40 Hz QPOs are detected in the same observations in 1997 July and November. However, the QPO is not detected in observations from 1996 April, May, and June in which the 67 Hz QPO was first discovered. The frequency of the 67 Hz QPO is significantly higher in the 1997 observations by about 5% compared with the 1996 data. The identification of the 40 Hz QPO makes GRS 1915ϩ105 the second black hole binary to show a pair of simultaneous high-frequency QPOs (the other being GRO J1655Ϫ40). The similarities between the properties of the 67 Hz QPO in GRS 1915ϩ105 and the recently discovered 450 Hz QPO in GRO J1655Ϫ40 suggest that the pairs of frequencies in these systems may be produced by the same physical mechanism, with the frequency differences between the two being likely due to different black hole masses in the two systems. We discuss the implications of our result for the mass and spin of GRS 1915ϩ105 as well as for models of X-ray variability in black holes and neutron stars.

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Rapid infrared flares in GRS 1915+105: evidence for infrared synchrotron emission

Cited by 113 publications

References 16 publications

On the optical extinction and distance of GRS 1915+105

On the optical extinction and distance of GRS 1915+105

Evidence for local mass accretion rate variations in the disc of GRS 1915+105

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

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