Milliarcsecond-resolution observations of IRC +10216

Details Milliarcsecond-resolution observations of IRC +10216 Milliarcsecond-resolution observations of IRC +10216

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003newa....8..507r&link_type=abstract

New Astronomy, Volume 8, Issue 6, p. 507-515.

Astronomy and Astrophysics

Astronomy

4

Occultations, Stars: Carbon, Circumstellar Matter, Stars: Individual: Irc +10216, Stars: Mass-Loss, Stars: Agb And Post-Agb

Scientific paper

We analyze two lunar occultation lightcurves of the carbon star IRC +10216 (CW Leo). The two events were recorded in 1989 and 1998, in the near-infrared H and K bands respectively. The results consist of two extended (~2''), high-resolution (~0''.001), one-dimensional brightness profiles along position angles 164° and 304° at the two epochs. The profiles show evidence for a bright central spike of emission having a FWHM of 0''.035, which is consistent with what is predicted by current models for the photosphere of the central star in IRC +10216. This feature can be identified with the so-called A component recently revealed by speckle imaging [A&A 334 (1998) L5; A&A 357 (2000) 169; A&A 333 (1998) L51], and the so-called core of the southern component observed with the aperture masking technique by Tuthill et al. [ApJ 543 (2000) 284]. The B component, alternatively suggested to mark the actual location of the central star by Osterbart et al. [A&A 357 (2000) 169], also seems to show a FWHM consistent with the above value, but it is well detected only in the 1998 K-band lightcurve, while for the 1989 H-band data the detection is less evident. Our brightness profiles also reveal a wealth of other structures, on several levels of scale, which are consistent with models of episodic dust ejection from the central star [A&A 302 (1995) 483].

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