81. A.G.A. The Death of

Brontë, Emily

doi:10.1093/oseo/instance.00209314

Cited by 19 publications

(26 citation statements)

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“…Such influence has been largely analysed from a theoretical point of view and recently studied, for stars hotter than those of the present paper, by Brown & Verschueren (1997). Fig.…”

Section: Rotational Velocitiesmentioning

confidence: 87%

Search for reference A0 dwarf stars: Masses and luminosities revisited with Hipparcos parallaxes

Gerbaldi

Faraggiana

Burnage

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract. Hipparcos data for 71 nearby dwarf A0 stars were combined with other data, in particular with high resolution spectra to establish the HR diagram in this temperature range. Almost 30% of unknown binaries were detected and discarded before establishing the M-L relation for bright A0 V field stars. The relationship derived for these single stars is compared to the classical diagram derived from eclipsing binaries. The scatter of the latter is examined and the role of gravity is discussed.A good agreement is found between the evolutionbased surface gravity log g ev and the value of log g ph obtained from photometric data.

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“…Such influence has been largely analysed from a theoretical point of view and recently studied, for stars hotter than those of the present paper, by Brown & Verschueren (1997). Fig.…”

Section: Rotational Velocitiesmentioning

confidence: 87%

Search for reference A0 dwarf stars: Masses and luminosities revisited with Hipparcos parallaxes

Gerbaldi

Faraggiana

Burnage

et al. 1999

Astron. Astrophys. Suppl. Ser.

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“…If it is a non-membeF, I obtain R = 5.31 -6.21 R©. Brown and Verschueren (1997) give v sin i = 260 k m s -1 while Stefl et al (1995) obtained v sin i = 335 km s _ 1 from high-dispersion spectra. For the latter value, an upper limit to the rotational period is 0?80 -0^93.…”

Section: Discussion Of a Few Often Studied Be Starsmentioning

confidence: 99%

“…H Cen (HR 5193, HD 120324) i s a very intensively studied B2e star (cf., e.g., Rivinius et al 1998). My values of M = 7.5 M© and R = 5.2 -5.4 R©, in combination with v sin i = 130 km s _ 1 (Brown and Verschueren 1997) give an upper limit to the rotational period of 2?06. n Cen (HR 5193, HD 120324) is another intensively studied B2e star, known for rapid changes with a period of 0?64.…”

Section: Discussion Of a Few Often Studied Be Starsmentioning

confidence: 99%

Physical Properties and Evolutionary Stage of Be Stars

Harmanec

2000

International Astronomical Union Colloquium

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The determination of accurate and reliable basic physical properties of Be stars is a very complicated task which, among other things, requires a good knowledge of the variability pattern of each particular object. Possible confusion between a rotationally distorted photosphere and a pseudophotosphere – an inner optically thick part of a gradually formed envelope which temporarily mimics a photosphere – is discussed in some detail in relation to the stellar effective temperature, brightness and rate of rotation. It is shown that the currently available data allow us to set relatively stringent limits on possible radii of at least some brighter Be stars, but very few direct determinations of mass have been made. The only exceptions are the Be stars in eclipsing binaries. The trouble is, however, that all of them are interacting binaries for which reliable orbital solutions are seriously hampered by the presence of gas streams and by strong interactions between the binary components. Moreover, their masses need not be representative for the whole population of Be stars.An answer to the question about the evolutionary stage of Be stars is even more uncertain since it is closely related to the principal, as yet unanswered question about the origin of the Be phenomenon itself.

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“…However this leads us to conclude possible differences in initial conditions of formation of Be and young Herbig Be stars because if classical Be stars were surrounded by dust shells in earlier evolutionary phases they would also have low v sin i values at present (see also discussion in Zorec & Briot 1997). A detailed discussion of various mechanisms for the redistribution of AM can be found in Brown & Verschueren (1997).…”

Section: Classical Be Starsmentioning

confidence: 94%

Analysis of correlations between polarimetric and photometric characteristics of young stars

Yudin¹

2000

Astron. Astrophys. Suppl. Ser.

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Abstract. We present the results of the investigation of correlations between the polarimetric and photometric characteristics of a sample (496 objects) of young Herbig Ae/Be (HAEBE) stars and T Tauri (TT) stars. It is shown that, for 85% of the sample stars there is a general relation between the degree of optical polarization and the infrared colour index (V − L) obs and the colour excess E(V − L) due to the contribution of a circumstellar dust shell. Polarimetric data were also compared with the value of v sin i to search for a possible correlation between the polarization and an inclination of circumstellar disks. Polarimetric data as well as IR excesses are considered and compared for different subgroups of young stars namely: HAEBE and TT stars with Algol-like minima of brightness (26 objects), Vega-type stars and post HAEBE stars (114 objects) and young solar-type stars (58 objects). For statistical purposes the data for young stars were compared with those collected for different groups of evolved objects such as: classical Be stars (≈300 objects), Mira Ceti stars (39 objects), early-type supergiants from the Serkowski et al. (1975) catalogue (120 objects) and main sequence (MS) stars within 50 pc from the Sun from the Leroy (1993) catalogue (68 objects). The value of polarization is discussed in context with the stages of evolution of circumstellar shells which were established by comparison of spectral energy distribution in the far IR (using the IRAS data). It is shown that most young stars have statistically larger value of polarization in comparison with the stars which are on a stage of evolution close to MS. We are able to contend that the changes in polarimetric behaviour of young stars are connected with evolution of their circumstellar shells.Appendices 1 to 5 are only available in electronic form at

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81. A.G.A. The Death of

Cited by 19 publications

References 0 publications

Search for reference A0 dwarf stars: Masses and luminosities revisited with Hipparcos parallaxes

Search for reference A0 dwarf stars: Masses and luminosities revisited with Hipparcos parallaxes

Physical Properties and Evolutionary Stage of Be Stars

Analysis of correlations between polarimetric and photometric characteristics of young stars

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