X-rays and Planet Formation

Details X-rays and Planet Formation X-rays and Planet Formation

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1855f&link_type=abstract

American Astronomical Society, HEAD meeting #9, #18.55; Bulletin of the American Astronomical Society, Vol. 38, p.391

Astronomy and Astrophysics

Astronomy

Scientific paper

While planets form in protoplanetary disks that are thermodynamically cool, X-rays from 10-100 MK plasma from their host pre-main sequence (PMS) stars can irradiate these disks affecting the processes of planet formation. This argument proceeds in three steps. First, Chandra studies of young stellar population show that PMS stars are typically 3 orders-of-magnitude more luminous in X-rays than old disk stars. Most of this emission is generated in violent magnetic reconnection events unrelated to accretion. Second, the recent Chandra Orion Ultradeep Project provides two lines of evidence (6.4 keV iron fluorescent emission; soft X-ray absorption in inclined proplyds) that X-rays do efficiently illuminate disks, at least in some cases. Third, theoretical studies show that PMS X-rays will then be the dominant source of disk gas ionization, and this ionization may induce MHD turbulence, gas-field coupling, gas heating, and astrochemical reactions which can have substantial effect on the processes of planetary formation and early evolution.

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