The β Pictoris circumstellar disk. XXI. Results from the December 1992 spectroscopic campaign.

Details The β Pictoris circumstellar disk. XXI. Results from the December 1992 spectroscopic campaign. The β Pictoris circumstellar disk. XXI. Results from the December 1992 spectroscopic campaign.

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...310..547l&link_type=abstract

Astronomy and Astrophysics, v.310, p.547-563

Astronomy and Astrophysics

Astrophysics

35

Stars: Circumstellar Matter, Stars: {Beta} Pictoris

Scientific paper

We present the results of an observational multisite and multiwavelength spectroscopic campaign performed in December 1992 on β Pic to test our Falling Evaporating Body scenario. The unprecedented sampling obtained enabled us to follow the β Pic variations from the ground over an 11-day period, and from the ground and space over a 5-day period. The evolution in terms of velocity and the timescales for variability are studied, and comparisons are made between various variable elements (CaII, MnII, FeII, AlIII and AlII). Very significant activity occurred throughout the campaign. We confirm the existence of two velocity regimes: low-velocity, slowly variable lines, and high-velocity, rapidly variable ones. It is shown that the higher the redshift, the smaller the variability timescale, the smaller the filling factors of the absorbing clouds, and the wider the lines. We detect for the first time the local effect of stellar rotation described by Beust & Lissauer (1994), which enables us to infer the location of the projection of the infalling absorbing cloud on the stellar surface. The variability of FeII appears to be correlated with that of CaII. Conversely, AlIII variability is not correlated with that of CaII. The observed evolution and characteristics of the high-velocity events appear to be well explained by the evaporation of one single body The evolution of the low-velocity variable events cannot be reproduced by the evaporation of one single body, but rather by a family of bodies on adjacent orbits.

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