Emission lines in the long-period Cepheid L Carinae

Details Emission lines in the long-period Cepheid L Carinae Emission lines in the long-period Cepheid L Carinae

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420..401b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 1, p. 401-414

Astronomy and Astrophysics

Astronomy

12

Carbon, Cepheid Variables, Emission Spectra, Periodic Variations, Shock Waves, Stellar Envelopes, Magnesium, Oxygen, Spectrum Analysis, Ultraviolet Astronomy

Scientific paper

For the Cepheid l Carinae, with a pulsation period of 35.5 days, we have studied the emission-line fluxes as a function of pulsational phase in order to find out whether we see chromospheric and transition-layer emission due to an outward-moving shock. All emission lines show a steep increase in flux shortly before maximum light, suggestive of a shock moving through the surface layers. The large ratio of C IV to C II line fluxes shows that these are not transition-layer lines. During maximum light the large ratio of the large ratio of the C IV to C II line fluxes also suggests that we see emission from a shock with velocities greater than 100 km/s such that C IV emission can be excited. With such velocities mass outflow appears possible. The variations seen in the MG II line profiles show that there is an external absorption over a broad velocity band independent of the pulsation phase. We attribute this absorption to a circumstellar 'shell.' This 'shell' appears to be seen also as spatially extended emission in the O I line at 1300 A, which is probably excited by resonance with Ly beta.

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