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2011ATel.3376....1S - The Astronomer's Telegram, 3376, 1 (2011/May-0)
Development of discrete velocity components in the optical spectrum of T Pyx.
SHORE S.N., AUGUSTEIJN T., EDEROCLITE A. and UTHAS H.
Abstract (from CDS):
but not other lines arising from the same level. The P Cyg absorption became more evident on the next spectrum, May 6.9 UT, for all of these
transitions showing detached components at progressively higher velocities. The Na I D line illustrates this evolution (Na I P Cyg profiles and their changes have been noted for only a few other novae, notably V705 Cas 1993): May 6.88 UT, -1900, -1160, -660 (weak); May 15.90 UT, -2000, -1350, -820;
May 21.87 UT: -2200 with numerous narrower components. The highest velocity feature is seen for only Na I D1 on all spectra with approximately constant FWHM ∼ 350±50 km/s and constant profile despite increasing velocity. The last spectrum appears to show a very broad emission component at +2000 to +3000 km/s. The velocity shifts and profiles are consistent with a linear velocity law for some form of continuous flow that is being occasionally loaded with mass by a source
that is pulsing, perhaps coincident with the events noted on the light curve in ATel 3373. If so, the forcing cannot be radiative, there is no evidence a terminal velocity, and the velocity gradient appears to be very steep near the temporary ``photosphere'' (see Shore et al. 1994, AJ, 108, 671 for the symbiotic system MWC 560). The individual narrow
components appear to be emerging as the broad absorption features become
progressively more transparent but were already present. Similar changes
to Na I D are seen on the Fe II RMT 42 profiles and Ca II.
Abstract Copyright: ∼
Journal keyword(s): Nova
Simbad objects: 3
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