The far UV spectrum of the Be star AX Monocerotis

Danezis, E.; Theodossiou, E.; Laskarides, P. G.

doi:10.1007/bf00642357

Cited by 13 publications

(9 citation statements)

References 7 publications

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“…Also, based on the Mg II absorption at 280 nm, they confirm the presence of a large amount of circumstellar matter. Danezis et al (1991) performed similar analyses of IUE spectra.…”

Section: Observational Historymentioning

confidence: 98%

Variability of the Hα spectral line in the interacting binary AX Monocerotis

Puss

Leedjärv

2002

A&A

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Abstract. The interacting binary system AX Mon (K-giant + B(e) star) has been observed at the Tartu Observatory, Estonia, from 1985 to 2000. In the present paper, mostly the behaviour of the hydrogen Hα line from 1996 to 2000 is investigated. We have found that the Hα profiles are variable on time scales from hours to years, with main features appearing around the conjunctions of the stars (K-star in front). Those features include weakening of the main absorption component of the P Cygni like profile and appearance of additional absorption and/or emission components. Occasionally, the Hα line as a whole shifts on the wavelength scale. All those effects seem to occur much stronger at every second conjunction, which we propose to call "strong" conjunctions. We propose that this variability is due to a gas cloud close to the Be star. This cloud is a region, where a stream of matter from the K-giant collides with the circumstellar gas from the Be-star. The mass transfer process seems to have become more unstable than in 1960s. It is possible that a cyclic behaviour of the Hα line with a periodicity of about two orbital periods is present.

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“…Also, based on the Mg II absorption at 280 nm, they confirm the presence of a large amount of circumstellar matter. Danezis et al (1991) performed similar analyses of IUE spectra.…”

Section: Observational Historymentioning

confidence: 98%

Variability of the Hα spectral line in the interacting binary AX Monocerotis

Puss

Leedjärv

2002

A&A

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“…Some years ago our group proposed a new model to explain the complex structure of the density regions of hot stars, where the spectral lines that present SACs or DACs are created (Danezis et al 1991(Danezis et al , 1998(Danezis et al , 2000a(Danezis et al ,b,c, 2002a(Danezis et al ,b,c, 2003, Laskarides et al 1992a,b).…”

Section: The Line Profile Functionmentioning

confidence: 99%

“…One of the most important phenomena in the spectra of hot emission stars is the DACs (Discrete Absorption Components) phenomenon (Peton 1974, Underhill 1975, Lamers et al 1982, Sahade et al 1984, Sahade & Brandi 1985, Hutsemékers 1985, Danezis 1984, 1987, Danezis et al 1991, 2003.…”

Section: Introductionmentioning

confidence: 99%

A New Modeling Approach For DACs And SACs Regions In The Atmospheres Of Hot Emissions Stars

Danezis¹,

Nikolaidis²,

Lyratzi³

et al. 2006

AIP Conference Proceedings

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The presence of Discrete Absorption Components (DACs) or Satellite Absorption Components (SACs) is a very common phenomenon in the atmospheres of hot emission stars (Danezis et al. 2003, Lyratzi & Danezis 2004) and result to the complex line profiles of these stars. The shapes of these lines are interpreted by the existence of two or more independent layers of matter nearby a star. These structures are responsible for the formation of a series of satellite components for each spectral line. Here we will present a model reproducing the complex profile of the spectral lines of Oe and Be stars with DACs and SACs (Danezis et al. 2003, Lyratzi & Danezis 2004. In general, this model has a line function for the complex structure of the spectral lines with DACs or SACs and include a function L that considers the kinematic (geometry) of an independent region. In the calculation of the function L we have considered the rotational velocities of the independent regions, as well as the random velocities within them. This means that the new function of L is a synthesis of the rotational distribution and a physical Gaussian. Finally, we calculate the optical depth (ξ) and the column density (d) of each independent density region.

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“…Many researchers have observed the existence of absorption components shifted to the blue or red wing of the main spectral line (e.g., Doazan 1982;Danezis et al 1991;Doazan et al 1991;Lyratzi et al 2007;Danezis et al 2007). In this paper, using the GR model ), we analyze the UV Mg II resonanse lines at λ = 2795.523 and 2802.698Å in the spectra of 20 Be stars of different spectral subtypes and present the values of the rotational, radial and random velocities, as well as the FWHM and the absorbed energy, as a function of the effective temperature of the studied stars.…”

Section: Introductionmentioning

confidence: 99%

Studying the UV Mg II Resonance Lines in 20 Be Stars

et al. 2011

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Abstract. Using the GR model, we analyze the UV Mg II resonance lines in the spectra of 20 Be stars of different spectral subtypes, in order to detect the presence of satellite or discrete absorption components. The values of some physical parameters -rotational, radial and random velocities, as well as the FWHM and the absorbed energy, as a function of the effective temperature for the studied stars are determined.

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The far UV spectrum of the Be star AX Monocerotis

Cited by 13 publications

References 7 publications

Variability of the Hα spectral line in the interacting binary AX Monocerotis

Variability of the Hα spectral line in the interacting binary AX Monocerotis

A New Modeling Approach For DACs And SACs Regions In The Atmospheres Of Hot Emissions Stars

Studying the UV Mg II Resonance Lines in 20 Be Stars

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