V 505 Mon: One of the most massive binaries

Stagni, R.; Margoni, R.; Mammano, A.

doi:10.1007/bf00648993

Cited by 7 publications

(4 citation statements)

References 8 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Stagni et al (1982) noted that all the old velocity measurements by Pearce & Petrie (1951) and Petrie & Pearce (1961), except the first one, are compatible with a pe- riod of 53. d 78. We remeasured the old plates and found good agreement with the original measurements, except again for the first one.…”

Section: Spectroscopy In the Optical Regionmentioning

confidence: 80%

See 1 more Smart Citation

V505 Mon -An early-type binary with a disk

Mayer

Chochol

Drechsel³

et al. 2001

A&A

View full text Add to dashboard Cite

Abstract. New spectra of the eclipsing binary V505 Mon (usually classified as B5 Ib) were obtained in the optical and UV regions. Only spectral lines of one component are visible, with K = 93 km s −1 . According to arguments based on the extent of the disk the mass ratio might be about 0.30. The star with the visible spectral lines would then have a mass of 2.3, the other component of 7.7 M , i.e. their supergiant nature can be ruled out. The distance to the system appears to be about 1 kpc. Together with published photometric data, the spectroscopy provides clear evidence for the presence of a disk around the secondary component. The profiles of the C ii 1335/6 doublet lines are used to derive the rotational velocity of the disk. The structure of the disk can be characterized by a central ionized zone surrounded by neutral outer parts. Additional matter of cloudy nature has to be present, and both components are embedded in an extended atmosphere. Abundance of carbon was found to be very low. Similarity with some other non-eclipsing binaries is discussed.

show abstract

Section: Spectroscopy In the Optical Regionmentioning

confidence: 80%

“…Initially, two possible values of the period -26. d 95 or 53. d 78 -were considered by Chochol & Kučera (1981); the longer value was later confirmed by the spectroscopic study of Stagni et al (1982). These authors analyzed low dispersion spectra, and the detection of secondary lines was claimed.…”

Section: Introductionmentioning

confidence: 85%

V505 Mon -An early-type binary with a disk

Mayer

Chochol

Drechsel³

et al. 2001

A&A

View full text Add to dashboard Cite

show abstract

“…V505 Mon was first reported as a photometric variable by Wachmann (1966). Chochol k Kucera (1981) detected the eclipses and found the orbital period 53.78 days confirmed by Stagni et al (1982) from low-dispersion spectroscopy. In Paper I, we determined the spectroscopic orbit of the primary component and brought photometric and spectroscopic evidence for the presence of a disk surrounding the secondary component.…”

Section: V505 Mon -An Early Type Binary With a Diskmentioning

confidence: 85%

Binaries with Invisible Massive Components

Chochol

Mayer

2002

International Astronomical Union Colloquium

View full text Add to dashboard Cite

V505 Mon is an early type eclipsing binary (usually classified as B5 Ib), in which only spectral lines of the primary component are visible. The radial velocity curve provides f(m) = 4.6 M⊙, suggesting that the secondary, invisible component is more massive. We have found evidence that this star is hidden from view by the disk detected during the primary eclipse. The structure of the disk can be characterized by a central ionization zone surrounded by the neutral outer parts. The profiles of the CII 1335/6 doublet lines were used to derive the rotational velocity of the disk as well as the velocity of the stream from the primary component to the disk. The masses of the components, deduced from the fractional size of the disk, are M1 = 1 M⊙ and M2 = 6.1 M⊙. Due to the low mass of the primary component its supergiant nature can be ruled out. Additional matter of a cloudy nature is present in the system and both components are embedded in an extended atmosphere. V505 Mon seems to be a prototype of the whole group of similar early-type binaries, in which the more massive component is hidden by a circumstellar medium, most likely a disk. Probable members are V742 Cas, V1362 Cyg, V2174 Cyg, V447 Sct and FY Vel with orbital periods between 33 and 225 days. Emission in Ha is always present, but there are no emissions in IUE spectra, so these binaries are distinct from the W Ser type. The evolutionary state of the members of this group is not yet understood.

show abstract

“…Early studies on the empirical MLRs for stars with masses larger than 0.6M pointed out that the slope of the MLR in the mass interval 1.5M < m < 2M exhibits a phenomenon of abrupt change [18,19,70,71] . Cester et al [18] and Demircan et al [19] described this phenomenon by introducing a critical mass and this mass was determined respectively as 1.5M and 1.7M .…”

Section: The Improved Mlrmentioning

confidence: 99%

The V-band Empirical Mass-luminosity Relation for Main Sequence Stars

Xia

2010

Chinese Astronomy and Astrophysics

View full text Add to dashboard Cite

V 505 Mon: One of the most massive binaries

Cited by 7 publications

References 8 publications

V505 Mon -An early-type binary with a disk

V505 Mon -An early-type binary with a disk

Binaries with Invisible Massive Components

The V-band Empirical Mass-luminosity Relation for Main Sequence Stars

Contact Info

Product

Resources

About