Poems (1640–1665)

Bradstreet, Anne

doi:10.1002/9780470693551.ch13

Cited by 2 publications

(3 citation statements)

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“…It is possible to model the observed light curve with a standard eclipsing binary code as included, for example, in the program Binary Maker 2.0 (Bradstreet 1992). A sophisticated approach is not needed here because effects such as reflection and distortion are negligible.…”

Section: An Eclipsing Binary Modelmentioning

confidence: 99%

An Unusual Eclipse of a Pre-Main-Sequence Star in IC 348

Cohen¹,

Herbst²,

Williams³

2003

ApJ

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A solar-like pre-main-sequence star (TJ 108pH187pLRLL 35pHMW 15) in the extremely young cluster IC 348 has been found, which apparently experienced an eclipse lasting ∼3.5 years, much longer than has ever been detected for any normal eclipsing binary. The light curve is flat-bottomed and rather symmetric, with a depth of 0.66 mag in Cousins I. During eclipse, the system reddened by ∼0.17 mag in RϪI. We argue that the eclipsing body is not a star because of the small probability of detecting an eclipse in what would be a very widely separated binary. Instead, it appears that the eclipse was caused by a circumstellar or circumbinary cloud or disk feature that occulted the star, or one of its components, if it is a binary system. We emphasize the importance of more detailed study of this object, which appears to be a new member of a small class of premain-sequence stars whose variability can be firmly linked to occultation by circumstellar (or circumbinary) matter.

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Section: An Eclipsing Binary Modelmentioning

confidence: 99%

An Unusual Eclipse of a Pre-Main-Sequence Star in IC 348

Cohen¹,

Herbst²,

Williams³

2003

ApJ

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show abstract

“…Several systems were excluded from the next analysis because some authors did not publish all parameters of the light curve fitting. If fill-out factor was not given, we computed it with the BinMaker 2.0 software (Bradstreet 1992) from the mass ratio and surface potential, but other missing results could not be reproduced by us. That is why these systems were omitted from the sample.…”

Section: Mass Ratio -Luminosity Ratio Relationmentioning

confidence: 99%

“…If the fill-out factor was not given, we computed it with the BinMaker 2.0 software (Bradstreet 1992) from the mass ratio and surface potential, but other missing results could not be reproduced by us. For this reason these systems were omitted from the sample.…”

Section: Mass Ratio -Luminosity Ratio Relationmentioning

confidence: 99%

On the properties of contact binary stars

Csizmadia¹,

Klagyivik²

2004

A&A

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Abstract.We have compiled a catalogue of light curve solutions of contact binary stars. It contains the results of 159 light curve solutions. The properties of contact binary stars were studied using the catalogue data. As is well known since Lucy's (1968a,b) and Mochnacki's (1981) studies, primary components transfer their own energy to the secondary star via the common envelope around the two stars. This transfer was parameterized by a transfer parameter (ratio of the observed and intrinsic luminosities of the primary star). We prove that this transfer parameter is a simple function of the mass and luminosity ratios. We introduced a new type of contact binary stars: H subtype systems which have a large mass ratio (q > 0.72). These systems show behaviour in the luminosity ratio-transfer parameter diagram that is very different from that of other systems and according to our results the energy transfer rate is less efficient in them than in other types of contact binary stars. We also show that different types of contact binaries have well defined locations on the mass ratio -luminosity ratio diagram. Several contact binary systems do not follow Lucy's relation (L 2 /L 1 = (M 2 /M 1 ) 0.92 ). No strict mass ratio -luminosity ratio relation of contact binary stars exists.

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Poems (1640–1665)

Cited by 2 publications

References 0 publications

An Unusual Eclipse of a Pre-Main-Sequence Star in IC 348

An Unusual Eclipse of a Pre-Main-Sequence Star in IC 348

On the properties of contact binary stars

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