Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734030t&link_type=abstract
American Astronomical Society, AAS Meeting #217, #340.30; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
1
Scientific paper
V1647 Ori is a low-mass, deeply-embedded, pre-main sequence star that gained notoriety in 2003 November when it was observed to undergo a strong optical/NIR eruption. V1647 Ori has undergone two optical/NIR outbursts in the last decade, both of which gradually faded over several months to years. These eruptions are thought to be the result of large-scale accretion events.
The X-ray evolution of each of these eruptions has been monitored through multi-epoch Chandra X-ray Observatory observations. We present analysis of five observations that followed the most recent eruption of 2008 August and analysis of the complete suite of CXO observations from 2002 through 2009. We find that V1647 Ori's X-ray flux is well correlated with optical and infrared observations for both epochs, suggesting that the primary X-ray generation mechanism for this star during optical/NIR outbursts is accretion.
Light curves of the recent observations (2008 September 18 - 2009 April 21) show V1647 Ori's X-ray flux was variable on short timescales. The pattern of X-ray median photon energy, mean count rate, and mean hardness ratio of these short-duration (few ks) events is very similar to those of the long-term (few months to years) variations, suggesting that the short-duration variability is also accretion-related.
The spectra are very well modeled with a single-temperature plasma subject to intervening hydrogen column density. With the hydrogen column density, plasma temperature, and chemical abundance freely varying, the models for the recent spectra converged to fits with a plasma temperature of 4-6 keV, a column density of 4-5 x 1022 cm-2, and a chemical abundance of about 0.8 solar. During the 2008-2009 epoch, the X-ray luminosity varied from a peak of 8 x 1030 ergs/s to a minimum of about 2 x 1030 ergs/s. This work was funded by a grant from NASA's Chandra X-ray Center.
Grosso Nicolas
Hamaguchi Kenji
Kastner Joel H.
Principe David
Richmond Michael
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