Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A

Mazeh, T.; Martín, E. L.; Goldberg, D.; Smith, H. A.

doi:10.1093/mnras/284.2.341

Cited by 12 publications

(12 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…To date, this is among the smallest known mass ratios for a detached main-sequence spectroscopic binary. Mazeh et al (1997), observing in the red part of the visual spectrum, derived mass ratios of 0.57^0.02 and 0.48^0.03 for two binaries.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Mazeh

Prato

Simon

et al. 2002

ApJ

View full text Add to dashboard Cite

This paper outlines an infrared spectroscopic technique to measure the radial velocities of faint secondaries in known single-lined binaries. The paper presents our H-band observations with the Cryogenic Echelle (CSHELL) and the Phoenix spectrographs and describes detections of three low-mass secondaries in main-sequence binaries, G147-36, G164-67, and HD 144284, with mass ratios of 0.562^0.011, 0.423^0.042, and 0.380^0.013, respectively. The latter is one of the smallest mass ratios derived to date for detached main-sequence stars.

show abstract

Section: Discussionmentioning

confidence: 99%

“…Table 4 is a summary of the mass ratios and masses estimated for the three binaries. The primary masses for G147-36 and G164-67 are from Carney et al (1994) and for HD 144284 from Mazeh et al (1997). The latter is based only on the spectral type of the system.…”

Section: Global Solution For Binary Parametersmentioning

confidence: 99%

Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Mazeh

Prato

Simon

et al. 2002

ApJ

View full text Add to dashboard Cite

show abstract

“…6. They all have q > 0.65, whereas only one SB1 lies beyond this limit: GJ 793.1, which was detected as SB2 according to Mazeh et al (1997). It is rather surprising that the limit in mass ratio does not seem related to K 1 √ 1 − e 2 .…”

Section: Sb1 Sb2mentioning

confidence: 95%

Multiplicity among solar–type stars

Halbwachs

Mayor²,

Udry³

et al. 2002

A&A

323

431

View full text Add to dashboard Cite

Abstract. Two CORAVEL radial velocity surveys -one among stars in the solar neighbourhood, the other in the Pleiades and in Praesepe -are merged to derive the statistical properties of main-sequence binaries with spectral types F7 to K and with periods up to 10 years. A sample of 89 spectroscopic orbits was finally obtained. Among them, 52 relate to a free-of-bias selection of 405 stars (240 field stars and 165 cluster stars). The statistics corrected for selection effects yield the following results: (1) No discrepancy is found between the binaries among field stars and the binaries in open cluster. The distributions of mass ratios, of periods, the period-eccentricity diagram and the binary frequencies are all within the same error intervals. (2) The distribution of mass ratios presents two maxima: a broad peak from q ≈ 0.2 to q ≈ 0.7, and a sharp peak for q > 0.8 (twins). Both are present among the early-type as well as among the late-type part of the sample, indicating a scale-free formation process. The peak for q > 0.8 gradually decreases when long-period binaries are considered. Whatever their periods, the twins have eccentricities significantly lower than the other binaries, confirming a difference in the formation processes. Twins could be generated by in situ formation followed by accretion from a gaseous envelope, whereas binaries with intermediate mass ratios could be formed at wide separations, but they are made closer by migration led by interactions with a circumbinary disk. (3) The frequency of binaries with P < 10 years is about 14%. (4) About 0.3% of binaries are expected to appear as false positives in a planet search. Therefore, the frequency of planetary systems among stars is presently 7 +4 −2 %. The extension of the distribution of mass ratios in the planetary range would result in a very sharp and very high peak, well separated from the binary stars with low mass ratios.

show abstract

“…Actually, just a few measurements of the secondary radial velocity are sufficient to allow the derivation of the mass ratio accurately. Mazeh et al (1997Mazeh et al ( , 2002 outlined an approach for extracting radial velocities of faint low-mass secondaries by moving into the red or the infrared, where the spectrum of the cooler companion is not so badly overwhelmed by the primary. This approach has been carried out in the pre-main-sequence domain with considerable success (Steffen et al 2001;Prato et al 2002aPrato et al , 2002b.…”

Section: Future Prospectsmentioning

confidence: 99%

On the Mass‐Ratio Distribution of Spectroscopic Binaries

Goldberg

Mazeh

Latham

2003

ApJ

View full text Add to dashboard Cite

In this paper we derive the mass-ratio and secondary-mass distributions of a large, well-defined, complete sample of 129 spectroscopic binaries with periods between 1 and 2500 days. The binaries, whose orbits were published recently, were detected by a systematic radial-velocity survey of a sample of more than 1400 large proper motion stars. Three features stand out in the mass-ratio distribution: a rise as the mass ratio goes down to q $ 0:2, a sharp drop below q $ 0:2, and a smaller peak at q $ 0:8. Another way to characterize the results is to state that the distribution includes two '' populations,'' one with a high asymmetric peak at q $ 0:2 and another with a smaller peak at q $ 0:8, while the minimum between the two populations is centered at q $ 0:55. The size of the binary sample allows us to divide it into two subsamples and look for differences in the mass-ratio distributions of the two subsamples. We performed two different divisions: one into Galactic halo versus disk populations, and the other into high-and low-mass primary stars (above and below 0.67 M ). The former division yields differences with moderate statistical significance of 88%, while the latter is more significant at a level of 97%. Our analysis suggests that the rise toward low mass ratios does not appear in the mass-ratio distribution of the halo binaries. The other separation shows a broad peak at mass ratio of q $ 0:8 1 for the subsample of binaries with low-mass primaries but no corresponding peak in the subsample with high-mass primaries. We discuss our findings and their application to theories of binary formation.

show abstract

Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A

Cited by 12 publications

References 1 publication

Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Infrared Detection of Low‐Mass Secondaries in Spectroscopic Binaries

Multiplicity among solar–type stars

On the Mass‐Ratio Distribution of Spectroscopic Binaries

Contact Info

Product

Resources

About