The triple system AT Mic AB + AU Mic in the β $\beta $ Pictoris association

Messina, S.; Leto, G.; Pagano, I.

doi:10.1007/s10509-016-2886-x

Cited by 4 publications

(5 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…-HIP 102141AB (AT Mic) The most recent photometric analysis of this system is presented by Messina et al (2016a). Our analysis of the first season of SuperWASP data, allowed us to measure the stellar rotation periods of both components.…”

Section: -2mass J20013718-3313139mentioning

confidence: 99%

“…Torres et al (2006) reported v sin i A = 10.1 km s −1 and v sin i B = 15.8 km s −1 for the components A and B, respectively; whereas Scholz et al (2007) determined v sin i A = 10.56 km s −1 and v sin i B = 17 km s −1 . The most recent photometric analysis of this system is presented by Messina et al (2016b). Our analysis of the first season of SuperWASP data, allowed us to measure the stellar rotation periods of both components.…”

Section: -Hip 88399mentioning

confidence: 99%

See 1 more Smart Citation

TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

Messina

Millward²,

Buccino

et al. 2017

A&A

View full text Add to dashboard Cite

Aims. We intended to compile the most complete catalog of bona fide members and candidate members of the β Pictoris association, and to measure their rotation periods and basic properties from our own observations, public archives, and exploring the literature. Methods. We carried out a multi-observatories campaign to get our own photometric time series and collected all archived public photometric data time series for the stars in our catalog. Each time series was analyzed with the Lomb-Scargle and CLEAN periodograms to search for the stellar rotation periods. We complemented the measured rotational properties with detailed information on multiplicity, membership, and projected rotational velocity available in the literature and discussed star by star. Results. We measured the rotation periods of 112 out of 117 among bona fide members and candidate members of the β Pictoris association and, whenever possible, we also measured the luminosity, radius, and inclination of the stellar rotation axis. This represents to date the largest catalog of rotation periods of any young loose stellar association. Conclusions. We provided an extensive catalog of rotation periods together with other relevant basic properties useful to explore a number of open issues, such as the causes of spread of rotation periods among coeval stars, evolution of angular momentum, and lithium-rotation connection.

show abstract

Section: -2mass J20013718-3313139mentioning

confidence: 99%

Section: -Hip 88399mentioning

confidence: 99%

TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

Messina

Millward²,

Buccino

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…AT Mic (AKA GJ 799 , HD 196982, HIP 102141, CD-32 16135, 2MASS J20415111-3226073) is a literature close binary system and is highly likely to be a distant companion to AU Mic (Adams et al 1927;Caballero 2009;Shaya & Olling 2011;Messina et al 2016) with an on-sky separation of 0.23 pc which equates to 47,000 au on the sky. The AT Mic AB binary have Gaia G magnitudes of 9.576±0.003 and 9.605±0.003 respectively, so the stars are of a similar brightness and type.…”

Section: At Mic Abmentioning

confidence: 99%

An ALMA Survey of M-dwarfs in the Beta Pictoris Moving Group with two new debris disc detections

Cronin-Coltsmann,

Kennedy,

Kral

et al. 2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Previous surveys in the far-infrared have found very few, if any, M-dwarf debris discs among their samples. It has been questioned whether M-dwarf discs are simply less common than earlier types, or whether the low detection rate derives from the wavelengths and sensitivities available to those studies. The highly sensitive, long-wavelength Atacama Large Millimetre/submillimetre Array (ALMA) can shed light on the problem. This paper presents a survey of M-dwarf stars in the young and nearby Beta Pictoris Moving Group with ALMA at Band 7 (880 μm). From the observational sample, we detect two new sub-mm excesses that likely constitute unresolved debris discs around GJ 2006 A and AT Mic A and model distributions of the disc fractional luminosities and temperatures. From the science sample of 36 M-dwarfs including AU Mic, we find a disc detection rate of 4/36 or 11.1$^{+7.4}_{-3.3}$ per cent that rises to 23.1$^{+8.3}_{-5.5}$ per cent when adjusted for completeness. We conclude that this detection rate is consistent with the detection rate of discs around G- and K-type stars and that the disc properties are also likely consistent with earlier type stars. We additionally conclude that M-dwarf stars are not less likely to host debris discs, but instead their detection requires longer wavelength and higher sensitivity observations than have previously been employed.

show abstract

“…AT Mic is believed to be a member of the β Pictoris association, with an age of ∼25 Myr (Messina et al 2017). The rotation periods of components A and B are 1.19 and 0.78 days, respectively (Messina et al 2016(Messina et al , 2017; the bolometric luminosities of components A and B have been estimated as 1.3 × 10 32 and 1.2 × 10 32 erg s −1 (0.034 and 0.031 L ☉ ), respectively (Messina et al 2017). Both components are known to be magnetically active (e.g., Gershberg et al 1999).…”

Section: Targetmentioning

confidence: 99%

“…Identifying the flaring and non-flaring (quiescent) time intervals in our observations is not straightforward, because of the above mentioned gaps in the light curves, and also because of a high activity level: AT Mic spends ∼25% of the time in a flaring state, according to Messina et al (2016), or even more than 50% of time, according to Kunkel (1970). We determined the quiescent background levels by iteratively fitting the light curves with linear functions and removing the data points that exceeded these fits by more than 1σ; this procedure effectively provides a linear fit to the lower envelope of a light curve.…”

Section: Light Curves: Overviewmentioning

confidence: 99%

X-Ray and Ultraviolet Flares on AT Microscopii Observed by AstroSat

Kuznetsov¹,

Karakotov²,

Chandrashekhar³

et al. 2022

Res. Astron. Astrophys.

View full text Add to dashboard Cite

We present observations of the active M-dwarf binary AT Mic (dM4.5e+dM4.5e) obtained with the orbital observatory AstroSat. During 20 ks of observations, in the far ultraviolet (130-180 nm) and soft X-ray (0.3-7 keV) spectral ranges, we detected both quiescent emission and at least five flares on different components of the binary. The X-ray flares were typically longer than and delayed (by 5-6 min) with respect to their ultraviolet counterparts, in agreement with the Neupert effect. Using X-ray spectral fits, we have estimated the parameters of the emitting plasma. The results indicate the presence of a hot multi-thermal corona with the average temperatures in the range of ∼7-15 MK and the emission measure of ∼(2.9-4.5)×1052 cm-3; both the temperature and the emission measure increased during the flares. The estimated abundance of heavy elements in the corona of AT Mic is considerably lower than at the Sun (∼0.18−0.34 of the solar photospheric value); the coronal abundance increased during the flares due to chromospheric evaporation. The detected flares had the energies of ∼1031-1032 erg; the energy-duration relations indicate the presence of magnetic fields stronger than in typical solar flares.

show abstract

The triple system AT Mic AB + AU Mic in the β $\beta $ Pictoris association

Cited by 4 publications

References 52 publications

TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

An ALMA Survey of M-dwarfs in the Beta Pictoris Moving Group with two new debris disc detections

X-Ray and Ultraviolet Flares on AT Microscopii Observed by AstroSat

Contact Info

Product

Resources

About