Flaring Activity of SgrA*: Adiabatic Expansion of Nonthermal Plasma

Details Flaring Activity of SgrA*: Adiabatic Expansion of Nonthermal Plasma Flaring Activity of SgrA*: Adiabatic Expansion of Nonthermal Plasma

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20911207y&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #112.07; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The compact radio source SgrA* at the Galactic center is known to be variable in radio, millimeter, near-IR and X-rays. The flaring activity in near-IR and X-rays is thought to arise from the inner 10 Schwarzschild radii of the 3-4 ×106 M&sun; black hole coincident with SgrA*. Recent VLA measurements showed the evidence of flaring activity with a duration of about two hours similar to that seen in sub-millimeter wavelengths. In addition, the light curves showed a possible time delay of about 20-40 minutes between the
43 and 23 GHz peak emission. To confirm the time delay picture, we recently re-observed Sgr A* with the VLA in several epochs including simultaneous observations with the CSO and Chandra. The light curves and their corresponding cross-correlation peak are consistent with the 43 GHz peak emission leading the 23 GHz peak emission. Sub-millimeter and X-ray light curves also support a similar picture. These measurements imply that the burst of emission is due to an expanding outflow, which cools on a dynamical time scale as it moves away from SgrA*. A simple model by van der Laan (1966) or a jet model can explain the behavior of SgrA*.

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