The X-Ray View of the Low-Mass Stars in the Solar Neighborhood

Schmitt, J. H. M. M.; Fleming, T. A.; Giampapa, M. S.

doi:10.1086/176149

Cited by 236 publications

(130 citation statements)

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“…We estimated the X-ray flux for 2MASS J0213+3648 AB by applying the relations of Schmitt, Fleming & Giampapa (1995) (2005), we find that 2MASS J0213+3648 AB fractional X-ray flux is similar to, if not higher than, Hyades M dwarf members and much higher than the vast majority of field M dwarfs. Using the method of Malo et al (2014), we calculated that 2MASS J0213+3648 A/B has log L x = 28.5 ± 0.6 ergs s −1 .…”

Section: The Age Of 2mass J0213+3648 Abmentioning

confidence: 93%

2MASS 0213+3648 C: A wide T3 benchmark companion to an an active, old M dwarf binary

Deacon

Magnier

Liu

et al. 2017

Mon. Not. R. Astron. Soc.

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We present the discovery of a 360 AU separation T3 companion to the tight (3.1 AU) M4.5+M6.5 binary 2MASS J02132062+3648506. This companion was identified using Pan-STARRS 1 data and, despite its relative proximity to the Sun (22.2 +6.4 −4.0 pc; Pan-STARRS 1 parallax) and brightness (J=15.3), appears to have been missed by previous studies due to its position near a diffraction spike in 2MASS. The close M dwarf binary has active X-ray and Hα emission and shows evidence for UV flares. The binary's weak GALEX UV emission and strong Na I 8200 Å Na absorption leads us to an age range of ∼1-10 Gyr. Applying this age range to evolutionary models implies the wide companion has a mass of 0.063±0.009 M ⊙ . 2MASS J02132+3648 C provides a relatively old benchmark close to the L/T transition and acts as a key, older comparison to the much younger early-T companions HN Peg B and GU Psc b.

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Section: The Age Of 2mass J0213+3648 Abmentioning

confidence: 93%

2MASS 0213+3648 C: A wide T3 benchmark companion to an an active, old M dwarf binary

Deacon

Magnier

Liu

et al. 2017

Mon. Not. R. Astron. Soc.

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“…This depends on the stellar mass loss rate and stellar wind speed that are poorly understood and hard to measure for M-stars. Here we estimate the mass loss rate from the nondetection of X-rays from GJ 581 by ROSAT implying log L x < 26.44 erg/s (Schmitt et al 1995). The correlation between X-ray surface flux and mass loss rate of GKM-type stars (Wood et al 2005) then yields the upper limit of 2Ṁ , where the solar mass loss rateṀ = 2 × 10 −14 M yr −1 .…”

Section: Collision Poynting-robertson and Stellar Wind Timescales Fomentioning

confidence: 94%

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Lestrade

Matthews

Sibthorpe

et al. 2012

A&A

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Debris disks have been found primarily around intermediate and solar mass stars (spectral types A-K) but rarely around low mass M-type stars. We have spatially resolved a debris disk around the remarkable M3-type star GJ 581 hosting multiple planets using deep PACS images at 70, 100 and 160 μm as part of the DEBRIS Program on the Herschel Space Observatory. This is the second spatially resolved debris disk found around an M-type star, after the one surrounding the young star AU Mic (12 Myr). However, GJ 581 is much older (2-8 Gyr), and is X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images and found that the best fit model is for a disk extending radially from 25 ± 12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper belt but it surrounds a low mass star (0.3 M ) and its fractional dust luminosity L dust /L * of ∼10 −4 is much higher. The inclination limits of the disk found in our analysis make the masses of the planets small enough to ensure the long-term stability of the system according to some dynamical simulations. The disk is collisionally dominated down to submicron-sized grains and the dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. We suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars. Finally, the known planets, of low masses and orbiting within 0.3 AU from the star, cannot dynamically perturb the disk over the age of the star, suggesting that an additional planet exists at larger distance that is stirring the disk to replenish the dust.

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“…The hard band corresponds to the count rate in PHA (Pulse Height Amplitude) channels from 52 to 201 (from ∼ 0.5 to 2.0 keV) and the soft band to PHA channels from 11 to 41 ( from ∼ 0.1 to 0.4 keV). To obtain the X-ray flux of a given star, we considered the calibrations of Schmitt et al (1995). In particular, we used the conversion factor to obtain the energy flux from the measured count rate which depends on HR: CF = (5.30HR + 8.31) × 10 −12 ergs cm −2 counts −1 (2.3) Ribas et al (2007) calculated a relationship between the age and X-ray luminosity for stars of different spectral types ( Fig.…”

Section: Age Determinationmentioning

confidence: 99%

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

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A mis padres y hermana AgraïmentsEn primer lloc vull agrair als meus directors de tesi, Jordi Isern i Enrique García-Berro, que em donessin l'oportunitat de realitzar el doctorat a l'IEEC (al CSIC i a la UPC), així com que em proporcionessin tot el suport necessari. Crec que he après moltes coses importants en aquestsúltims anys, no només en la part científica, i això en partés una conseqüència d'haver treballat amb ells. Els vull donar les gràcies també pel suport i la confiança dipositada en mi, especialment durant aquestúltim any de feina.Durant tota aquestaèpoca he tingut la sort de tenir uns companys fantàstics que m'han fet molt més fàcil la feina. Primer vaig conèixer l'Alina, la meva companya de "fatigas" i després el Jose, el Pep i el Miquel. Més tard s'hi van afegir l'Ignasi, la Violeta, l'Anna C., l'Anna A., el Carlo, el Moi, el Nil, l'Anaïs. . . Tots els moments que hem compartit dins i fora de l'IEEC han estat molt importants per a mi i m'emporto un gran record de tota aquestaèpoca, primer al Nexus, després a la UAB i finalment a l'ETSE. Ara que tinc la oportunitat, els hi vull agrair als meus companys, o més ben dit, amics, tots elsànims i suport que m'han donat. També els hi vull donar les gràcies al personal d'administració i a la resta de companys que he tingut durant aquests anys.En especial, l'Ignasi es mereix un gran gràcies. . . Primer de tot, per venir a l'IEEC en un moment en que la meva feina necessitava d'un observador amb experiència. Per tenir la generositat de compartir els seus coneixements amb mi durant aquests anys, per acompanyar-me en les observacions, per tenir sempre tanta confiança en mi, molta més que jo mateixa i per ajudar-me sempre que se li presentés la oportunitat. Els seusànims i el seu suport han estat essencials per a que arribés aquest moment i per tant, només em queda donar-li el meu agraïment més sincer.También le debo un agradecimiento especial a Carlos Allende Prieto, que sin ni siquiera conocerme en persona aceptó acompañarme a observar al McDonald Observatory durante 10 días. Su ayuda y dedicación en la distancia, especialmente en el análisis de las compañeras de las enanas blancas, han sido también vitales para el desarrollo de esta tesis.Durante mi doctorado he tenido la oportunidad de disfrutar de estancias en otros centros. Le quiero dar las gracias a Inma Domínguez, Carlos Abia y Olga Zamora de la Universidad de Granada por la atención que me dispensaron cuando estuve allí. También quisiera dar las gracias a Roberto Silvotti y Juan Alcalá por la ayuda y el buen trato que me dieron durante el tiempo que pasé en el Osservatorio Astronomico di Capodimonte. Gracias también al resto de personas que trabajan en el Osservatorio y que hicieron mi estancia muy agradable.A mi profesor Manolo Segura le quiero agredecer que en su día me hiciera creer en mis posibilidades y despertara mi afán por intentar superarme poco a poco. Muchas gracias también por la "contingencia" y por la confianza dipositada en mí.En un momento para mí tan importante comoéste no me puedo olvi...

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The X-Ray View of the Low-Mass Stars in the Solar Neighborhood

Cited by 236 publications

References 0 publications

2MASS 0213+3648 C: A wide T3 benchmark companion to an an active, old M dwarf binary

2MASS 0213+3648 C: A wide T3 benchmark companion to an an active, old M dwarf binary

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Testing the Initial–Final Mass Relationship of White Dwarfs

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