SIMBAD references

2014ApJ...786..136D - Astrophys. J., 786, 136 (2014/May-2)

Burn out or fade away? on the X-ray and magnetic death of intermediate mass stars.

DRAKE J.J., BRAITHWAITE J., KASHYAP V., GUNTHER H.M. and WRIGHT N.J.

Abstract (from CDS):

The nature of the mechanisms apparently driving X-rays from intermediate mass stars lacking strong convection zones or massive winds remains poorly understood, and the possible role of hidden, lower mass close companions is still unclear. A 20 ks Chandra HRC-I observation of HR 4796A, an 8 Myr old main sequence A0 star devoid of close stellar companions, has been used to search for a signature or remnant of magnetic activity from the Herbig Ae phase. X-rays were not detected and the X-ray luminosity upper limit was LX ≤ 1.3x1027 erg/s. The result is discussed in the context of various scenarios for generating magnetic activity, including rotational shear and subsurface convection. A dynamo driven by natal differential rotation is unlikely to produce observable X rays, chiefly because of the difficulty in getting the dissipated energy up to the surface of the star. A subsurface convection layer produced by the ionization of helium could host a dynamo that should be effective throughout the main sequence but can only produce X-ray luminosities of the order 1025 erg/s. This luminosity lies only moderately below the current detection limit for Vega. Our study supports the idea that X-ray production in Herbig Ae/Be stars is linked largely to the accretion process rather than the properties of the underlying star, and that early A stars generally decline in X-ray luminosity at least 100,000 fold in only a few million years.

Abstract Copyright:

Journal keyword(s): stars: activity - stars: coronae - stars: magnetic field - Sun: activity - Sun: corona - X-rays: stars

Simbad objects: 10

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2014ApJ...786..136D and select 'bookmark this link' or equivalent in the popup menu


2019.09.23-09:59:33

© Université de Strasbourg/CNRS

    • Contact