The Helium Anomaly in ø Persei.

Hynek, J. A.

doi:10.1086/144652

Cited by 8 publications

(12 citation statements)

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“…I thus prefer Suzuki's interpretation of the effect. Suzuki applied his model of stable orbits to Hynek's (1940Hynek's ( ,1944) measurements of vp Per. Assuming sin i = 1, he arrived at the values of m^=20 and m^=4 for the masses of both stars, in excellent agreement with the above-mentioned result of Pcackert (1981)!…”

Section: F the Light And Spectral Variations (Often Pseudoperiodic)mentioning

confidence: 99%

Rotation, Expansion and Duplicity of Be Stars

Harmanec

1982

Symp. - Int. Astron. Union

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In recent years there is a general tendency to divide Be stars into different groups. Bidelman's (1976) division on supergiants, rapidly rotating single stars, interacting binaries, early type nebular variables and quasi (or young) planetary nebulae is often quoted. Another example is the classification by Lesh (1968) or a very recent classification by Jaschek et al (1980), limited a priori to “normal” Be stars i.e. stars of luminosity classes V to III. I do not think such an approach is recommendable. There is still no general agreement as to the nature of the Be phenomenon and all such classifications must be more or less descriptive. The possibility that the hydrogen emission observed in the spectra of apparently very different objects has always the same physical cause, and that the differences between these objects are caused only by continuously varying physical and/or geometrical parameters should seriously be considered, along with all other concepts. At the moment, I find it more promising to study Be stars in context of all early type emission objects, including supergiants, P Cyg stars, Beta Cep objects, WR stars, symbiotic stars and novae. Such a viewpoint is not new – it was expressed already by Struve (1942).

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Section: F the Light And Spectral Variations (Often Pseudoperiodic)mentioning

confidence: 99%

Rotation, Expansion and Duplicity of Be Stars

Harmanec

1982

Symp. - Int. Astron. Union

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“…He also pointed out that there were secular variations in the spectrum in addition to the cyclic changes. Hynek (1940), after a very comprehensive study of <j> Per, concluded that the star was a double-lined spectroscopic binary and that double He i lines, present during some phases, were due to two early-type stars. The double-lined spectroscopic binary hypothesis still left some peculiar spectrum variations unexplained.…”

Section: Introductionmentioning

confidence: 99%

“…He pointed out that the spectra show clear evidence for circumstellar gas and that most of the lines measured by Hynek originate in this gas, not in the stellar photosphere, and consequently the radial velocities found by Hynek did not necessarily pertain to the stars in the system. Hynek (1944) addressed himself to these peculiar variations (anomalous He i line-strength variations) and suggested that they might be explained by a hot gas cloud within the system.…”

Section: Introductionmentioning

confidence: 99%

A spectroscopic study of the binary Be star Phi Persei

Poeckert

1981

PASP

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High-dispersion high signal-to-noise ratio spectrograms of 4> Per have been obtained. The radial velocities of various spectral features have been measured and an orbit solution obtained. The (j> Persei system is found to consist of a 21 W© star, whose Vsin i is 450 km s -1 , and a 3.4 S .W© secondary. The secondary is peculiar in that Hell À4686 emission arises from within its vicinity. It is suggested that the secondary is the helium core of a once more massive star, its mass having been transferred to the primary. Both stars in the system have circumstellar disks and the dimensions of these disks are discussed.

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“…I was not the first to see them; they were first measured by Whitt, later by Hynek (1944), and most recently oscilloscopically by Hickok (1969). Further, the precaution was taken in the measures of not calculating phases until after the radial velocity reductions were completed.…”

Section: Observationsmentioning

confidence: 99%

“…Interest in the star <f> Persei -which lay largely dormant since the papers of Hynek in the 1940's (Hynek, 1940(Hynek, , 1944)-has recently begun to emerge again among investigators of the Be and shell phenomenon. This enigmatic star exemplifies in many ways the problems which beset astronomers studying these types of starsnamely, it is a spectrum and radial velocity variable.…”

Section: Introductionmentioning

confidence: 99%

Toward a Model for the Be Binary System φ Per

Hendry

1976

Symp. - Int. Astron. Union

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Arguments are presented against the adoption of an early B-red giant combination for the Persei system. Velocity curves of the primary and secondary components based on the measures of the He I lines on nearly two hundred plates are shown and discussed insofar as orbital parameters and system membership are concerned. Evidence from the He i lines, the emission edges, shell absorptions, and underlying wide absorptions of the hydrogen lines indicate that the system is made up of a Bl primary and a B3 secondary, both of which are emission-line stars.

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The Helium Anomaly in ø Persei.

Cited by 8 publications

References 0 publications

Rotation, Expansion and Duplicity of Be Stars

Rotation, Expansion and Duplicity of Be Stars

A spectroscopic study of the binary Be star Phi Persei

Toward a Model for the Be Binary System φ Per

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