New Challenges for Wind Shock Models: The Chandra Spectrum of the Hot Star δ Orionis

Details New Challenges for Wind Shock Models: The Chandra Spectrum of the Hot Star δ Orionis New Challenges for Wind Shock Models: The Chandra Spectrum of the Hot Star δ Orionis

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...577..951m&link_type=abstract

The Astrophysical Journal, Volume 577, Issue 2, pp. 951-960.

Astronomy and Astrophysics

Astronomy

57

Line: Profiles, Stars: Early-Type, Stars: Individual: Constellation Name: Δ Orionis, Stars: Mass Loss, Stars: Winds, Outflows, X-Rays: Stars

Scientific paper

The Chandra spectrum of δ Ori A shows emission lines from hydrogen- and helium-like states of Si, Mg, Ne, and O, along with N VII Lyα and lines from ions in the range Fe XVII-Fe XXI. In contrast to the broad lines seen in ζ Pup and ζ Ori (850+/-40 and 1000+/-240 km s-1 half-width at half-maximum [HWHM], respectively), these lines are broadened to only 430+/-60 km s-1 HWHM. This is much lower than the measured wind terminal velocity of 2000 km s-1. The forbidden, intercombination, and resonance (fir) lines from He-like ions indicate that the majority of the X-ray line emission does not originate at the base of the wind, in agreement with the standard wind shock models for these objects. However, in that model the X-ray emission is distributed throughout an expanding, X-ray-absorbing wind, and it is therefore surprising that the emission lines appear relatively narrow, unshifted, and symmetric. We compare the observed line profiles to recent detailed models for X-ray line profile generation in hot stars, but none of them offers a fully satisfactory explanation for the observed line profiles.

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