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Deciphering the X-ray Emission of the Nearest Herbig Ae StarIn this research program, we obtained and analyzed an X-ray observation of the young nearby intermediate mass pre-main sequence star HD 104237 using the XMM-Newton space-based observatory. The observation was obtained on 17 Feb. 2002. This observation yielded high-quality X-ray images, spectra, and timing data which provided valuable information on the physical processes responsible for the X-ray emission. This star is a member of the group of so-called Herbig Ae/Be stars, which are young intermediate mass (approx. 2 - 4 solar masses) pre-main sequence (PMS) stars a few million years old that have not yet begun core hydrogen burning. The objective of the XMM-Newton observation was to obtain higher quality data than previously available in order to constrain possible X-ray emission mechanisms. The origin of the X-ray emission from Herbig Ae/Be stars is not yet known. These intermediate mass PMS stars lie on radiative tracks and are not expected to emit X-rays via solar-like magnetic processes, nor are their winds powerful enough to produce X-rays by radiative wind shocks as in more massive O-type stars. The emission could originate in unseen low-mass companions, or it may be intrinsic to the Herbig stars themselves if they still have primordial magnetic fields or can sustain magnetic activity via a nonsolar dynamo.
Document ID
20040082517
Acquisition Source
Headquarters
Document Type
Contractor or Grantee Report
Authors
Skinner, Stephen L.
(Colorado Univ.)
Date Acquired
September 8, 2013
Publication Date
January 1, 2004
Subject Category
Astrophysics
Funding Number(s)
CONTRACT_GRANT: NAG5-10326
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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