Chandra observation of an unusually long and intense X-ray flare from a young solar-like star in M 78

¹ Max-Planck-Institut für extraterrestrische Physik, PO Box 1312, 85741 Garching bei München, Germany
² Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, 38041 Grenoble Cedex 9, France
³ Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA
⁴ Institute for the Study of Earth, Oceans, and Space, 39 College Road, University of New Hampshire, Durham, NH 03824, USA

Corresponding author: N. Grosso, Nicolas.Grosso@obs.ujf-grenoble.fr

Received: 11 July 2003
Accepted: 29 January 2004

Abstract

LkHα 312 has been observed serendipitously with the ACIS-I detector on board the Chandra X-ray Observatory with a 26 h continuous exposure. This Hα emission line star belongs to M 78 (NGC 2068), one of the star-forming regions of the Orion B giant molecular cloud at a distance of 400 pc. From the optical and the near-infrared (NIR) data, we show that LkHα 312 is a pre-main sequence (PMS) low-mass star with a weak NIR excess. This genuine T Tauri star displayed an X-ray flare with an unusually long rise phase (~8 h). The X-ray emission was nearly constant during the first 18 h of the observation, and then increased by a factor of 13 during a fast rise phase (~2 h), and reached a factor of 16 above the quiescent X-ray level at the end of a gradual phase (~6 h) showing a slower rise. To our knowledge this flare, with ~0.4–0.5 cts s^-1, has the highest count rate observed so far with Chandra from a PMS low-mass star. By chance, the source position, off-axis, protected this observation from pile-up. We make a spectral analysis of the X-ray emission versus time, showing that the plasma temperature of the quiescent phase and the flare peak reaches 29 MK and 88 MK, respectively. The quiescent and flare luminosities in the energy range 0.5–8 keV corrected from absorption ( cm^-2) are erg s^-1 and ~10³² erg s^-1, respectively. The ratio of the quiescent X-ray luminosity on the LkHα 312 bolometric luminosity is very high with , implying that the corona of LkHα 312 reached the “saturation” level. The X-ray luminosity of the flare peak reaches ~2% of the stellar bolometric luminosity. The different phases of this flare are finally discussed in the framework of solar flares, which leads to the magnetic loop height from to 10¹¹ cm (0.2–0.5 , i.e., 0.5–1.3 ).