The magnetically-active, low-mass, triple system WDS 19312+3607

Caballero, J. A.; Montes, D.; Klutsch, A.; Genebriera, J.; Miret, F. X.; Tobal, T.; Cairol, J.; Pedraz, S.

doi:10.1051/0004-6361/201014419

Cited by 5 publications

(4 citation statements)

References 48 publications

(76 reference statements)

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“…I19312+3607 itself is noted as a very close (<0.01 AU) double-lined spectroscopic binary in Shkolnik et al (2010). Additionally, there is a wide common proper motion companion at 46 ′′ (Caballero 2010).…”

Section: I18427+1354 (Gj 4071)mentioning

confidence: 96%

The Astralux Multiplicity Survey: Extension to Late M-Dwarfs

Janson

Bergfors

Brandner

et al. 2014

ApJ

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The distribution of multiplicity among low-mass stars is a key issue to understanding the formation of stars and brown dwarfs, and recent surveys have yielded large enough samples of nearby low-mass stars to study this issue statistically to good accuracy. Previously, we have presented a multiplicity study of ∼700 early/mid M-type stars observed with the AstraLux high-resolution Lucky Imaging cameras. Here, we extend the study of multiplicity in M-type stars through studying 286 nearby mid/late M-type stars, bridging the gap between our previous study and multiplicity studies of brown dwarfs. Most of the targets have been observed more than once, allowing us to assess common proper motion to confirm companionship. We detect 68 confirmed or probable companions in 66 systems, of which 41 were previously undiscovered. Detections are made down to the resolution limit of ∼100 mas of the instrument. The raw multiplicity in the AstraLux sensitivity range is 17.9%, leading to a total multiplicity fraction of 21-27% depending on the mass ratio distribution, which is consistent with being flat down to mass ratios of ∼0.4, but cannot be stringently constrained below this value. The semi-major axis distribution is well represented by a log-normal function with µ a = 0.78 and σ a = 0.47, which is narrower and peaked at smaller separations than for a Sun-like sample. This is consistent with a steady decrease in average semi-major axis from the highest-mass binary stars to the brown dwarf binaries.

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Section: I18427+1354 (Gj 4071)mentioning

confidence: 96%

The Astralux Multiplicity Survey: Extension to Late M-Dwarfs

Janson

Bergfors

Brandner

et al. 2014

ApJ

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“…Most prominently, the level of stellar activity may cause such a bias. For example, Caballero et al (2010), Jackson et al (2018), and Kesseli et al (2018) reported inflated radii for young, magnetically active, or fast rotating stars.…”

Section: Introductionmentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Schweitzer

Passegger

Cifuentes

et al. 2019

A&A

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186

177

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Aims. We determine the radii and masses of 293 nearby, bright M dwarfs of the CARMENES survey. This is the first time that such a large and homogeneous high-resolution (R > 80 000) spectroscopic survey has been used to derive these fundamental stellar parameters. Methods. We derived the radii using Stefan-Boltzmann's law. We obtained the required effective temperatures T eff from a spectral analysis and we obtained the required luminosities L from integrated broadband photometry together with the Gaia DR2 parallaxes. The mass was then determined using a mass-radius relation that we derived from eclipsing binaries known in the literature. We compared this method with three other methods: (1) We calculated the mass from the radius and the surface gravity log g, which was obtained from the same spectral analysis as T eff . (2) We used a widely used infrared mass-magnitude relation. (3) We used a Bayesian approach to infer stellar parameters from the comparison of the absolute magnitudes and colors of our targets with evolutionary models. Results. Between spectral types M0 V and M7 V our radii cover the range 0.1 R < R < 0.6 R with an error of 2-3% and our masses cover 0.09 M < M < 0.6 M with an error of 3-5%. We find good agreement between the masses determined with these different methods for most of our targets. Only the masses of very young objects show discrepancies. This can be well explained with the assumptions that we used for our methods.Article published by EDP Sciences A68, page 1 of 16 A&A 625, A68 (2019)

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“…Spectropolarimetry is conducted in combination with the grisms 400 Å/mm, 200 Å/mm, and 100 Å/mm. Apart from GRB follow-ups, CAFOS is contributing to SNe [242], binary star [243], and galaxy studies.…”

Section: Caha/cafosmentioning

confidence: 99%

Key Space and Ground Facilities in GRB Science

et al. 2022

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Gamma-ray bursts (GRBs) are short and intense flashes of γ-rays coming from deep space. GRBs were discovered more than a half century ago and now are observed across the whole electromagnetic spectrum from radio to very-high-energy gamma rays. They carry information about the powerful energy release during the final stage of stellar evolution, as well as properties of matter on the way to the observer. At present, space-based observatories detect on average approximately one GRB per day. In this review, we summarize key space and ground facilities that contribute to the GRB studies.

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The magnetically-active, low-mass, triple system WDS 19312+3607

Cited by 5 publications

References 48 publications

The Astralux Multiplicity Survey: Extension to Late M-Dwarfs

The Astralux Multiplicity Survey: Extension to Late M-Dwarfs

The CARMENES search for exoplanets around M dwarfs

Key Space and Ground Facilities in GRB Science

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