Navegar

Colección

Datos Estadísticas

Artículo

Messina, S.; Santallo, R.; Tan, T.G.; Elliott, P.; Feiden, G.A.; Buccino, A.; Mauas, P.; Petrucci, R.; Jofré, E. "Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association" (2017) Astronomy and Astrophysics. 601
Estamos trabajando para incorporar este artículo al repositorio
Consulte el artículo en la página del editor
Consulte la política de Acceso Abierto del editor

Abstract:

Context. There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. Aims. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. Results. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity. © ESO, 2017.

Registro:

Documento: Artículo
Título:Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association
Autor:Messina, S.; Santallo, R.; Tan, T.G.; Elliott, P.; Feiden, G.A.; Buccino, A.; Mauas, P.; Petrucci, R.; Jofré, E.
Filiación:INAF-Catania Astrophysical Observatory, via S.Sofia, 78, Catania, 95123, Italy
Southern Stars Observatory, Pamatai, Tahiti, French Polynesia, French, France
Perth Exoplanet Survey Telescope, Perth, 6000, Australia
European Southern Observatory, Alonso de Cordova 3107, Vitacura Casilla 19001, Santiago 19, Chile
School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, United Kingdom
Department of Physics, University of North Georgia, 82 College Circle, Dahlonega, GA 30597, United States
Instituto de Astronomía y Física Del Espacio (IAFE-CONICET), Buenos Aires, Argentina
Observatorio Astronómico de Córdoba, Laprida 854, Córdoba, X5000BGR, Argentina
Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina
Palabras clave:Binaries: general; Stars: activity; Stars: late-type; Stars: low-mass; Starspots; Bins; Lithium; Magnetism; Binaries: general; Stars: activity; Stars: low mass; Stars:late type; Starspots; Stars
Año:2017
Volumen:601
DOI: http://dx.doi.org/10.1051/0004-6361/201628514
Título revista:Astronomy and Astrophysics
Título revista abreviado:Astron. Astrophys.
ISSN:00046361
CODEN:AAEJA
Registro:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v601_n_p_Messina

Referencias:

  • Allard, F., Homeier, D., Freytag, B., (2012) Phil. Trans. R Soc. Lond. Ser. A, 370, p. 2765
  • Asplund, M., Grevesse, N., Sauval, A.J., Scott, P., (2009) ARA&A, 47, p. 481
  • Bailey, J.I., III, White, R.J., Blake, C.H., (2012) ApJ, 749, p. 16
  • Baraffe, I., Homeier, D., Allard, F., Chabrier, G., (2015) A&A, 577, p. A42
  • Bayo, A., Rodrigo, C., Barrado, Y., Navascués, D., (2008) A&A, 492, p. 277
  • Beers, T.C., Rossi, S., Ulrich, D., Wilhelm, R., (1996) AJ, 112, p. 1188
  • Bianchi, L., Kang, Y.B., Efremova, B., (2011) Ap&SS, 335, p. 249
  • Biller, B.A., Liu, M.C., Wahhaj, Z., (2013) ApJ, 777, p. 160
  • Binks, A.S., Jeffries, R.D., (2014) MNRAS, 438, p. L11
  • Binks, A.S., Jeffries, R.D., (2016) MNRAS, 455, p. 3345
  • Bouvier, J., Lanzafame, A.C., Venuti, L., (2016) A&A, 590, p. A78
  • Casagrande, L., Flynn, C., Bessell, M., (2008) MNRAS, 389, p. 585
  • Christian, D.J., Mathioudakis, M., (2002) AJ, 123, p. 2796
  • Cox, A.N., (2000) Allen's Astrophysical Quantities, , New York: AIP Press, Springer)
  • Cutri, R.M., Skrutskie, M.F., Van Dyk, S., (2003) The IRSA 2MASS All-Sky Point Source Catalog, NASA/IPAC Infrared Science Archive
  • Cutri, R.M., (2013) VizieR Online Data Catalog: II/328
  • D'Antona, F., Mazzitelli, I., (1997) Mem. Soc. Astron. Ital, 68, p. 807
  • Delorme, P., Collier Cameron, A., Hebb, L., (2011) MNRAS, 413, p. 2218
  • Delorme, P., Lagrange, A.M., Chauvin, G., (2012) A&A, 539, p. A72
  • Eggenberger, P., Haemmerlé, L., Meynet, G., Maeder, A., (2012) A&A, 539, p. A70
  • Elliott, P., Bayo, A., Melo, C.H.F., (2014) A&A, 568, p. A26
  • Elliott, P., Huélamo, N., Bouy, H., (2015) A&A, 580, p. A88
  • Elliott, P., Bayo, A., Melo, C.H.F., (2016) A&A, 590, p. A13
  • Feiden, G.A., (2016) A&A, 593, p. A99
  • Brown, A.G.A., (2016) A&A, 595, p. A2. , Gaia Collaboration
  • Høg, E., Fabricius, C., Makarov, V.V., (2000) A&A, 355, p. L27
  • Jackson, R.J., Jeffries, R.D., (2014) MNRAS, 445, p. 4306
  • Jayawardhana, R., Coffey, J., Scholz, A., Brandeker, A., Van Kerkwijk, M.H., (2006) ApJ, 648, p. 1206
  • Koen, C., Kilkenny, D., Van Wyk, F., Marang, F., (2010) MNRAS, 403, p. 1949
  • Kunkel, W.E., (1972) Information Bulletin on Variable Stars, 748
  • Lagrange, A.-M., Meunier, N., Chauvin, G., (2013) A&A, 559, p. A83
  • Lamm, M.H., Bailer-Jones, C.A.L., Herbstw, M.R., Scholz, A., (2004) A&A, 417, p. 557
  • Macdonald, J., Mullan, D.J., (2010) ApJ, 723, p. 1599
  • Malo, L., Artigau, E., Doyon, R., (2014) ApJ, 788, p. 81
  • Malo, L., Doyon, R., Feiden, G.A., (2014) ApJ, 792, p. 37
  • Mamajek, E.E., Bell, C.P.M., (2014) MNRAS, 445, p. 2169
  • Mamajek, E.E., Hillenbrand, L.A., (2008) ApJ, 687, p. 1264
  • Mentuch, E., Brandeker, A., Van Kerkwijk, M.H., Jayawardhana, R., Hauschildt, P.H., (2008) ApJ, 689, p. 1127
  • Messina, S., Desidera, S., Turatto, M., Lanzafame, A.C., Guinan, E.F., (2010) A&A, 520, p. A15
  • Messina, S., Lanzafame, A.C., Feiden, G.A., (2016) A&A, 596, p. A29
  • Messina, S., Millward, M., Buccino, A., (2017) A&A, 600, p. A83
  • Messina, S., Lanzafame, A.C., Malo, L., A&A (2017) Submitted
  • Pecaut, M.J., Mamajek, E.E., (2013) ApJS, 208, p. 9
  • Petrucci, R., Jofré, E., Schwartz, M., (2013) ApJ, 779, p. L23
  • Pojmanski, G., (1997) Acta Astron, 47, p. 467
  • Pojmanski, G., (2002) Acta Astron, 52, p. 397
  • Roberts, D.H., Lehar, J., Dreher, J.W., (1987) AJ, 93, p. 968
  • Roeser, S., Demleitner, M., Schilbach, E., (2010) AJ, 139, p. 2440
  • Scargle, J.D., (1982) ApJ, 263, p. 835
  • Shkolnik, E., Liu, M.C., Reid, I.N., (2009) ApJ, 699, p. 649
  • Shkolnik, E.L., Anglada-Escudé, G., Liu, M.C., (2012) ApJ, 758, p. 56
  • Siess, L., Dufour, E., Forestini, M., (2000) A&A, 358, p. 593
  • Soderblom, D.R., Jones, B.F., Balachandran, S., (1993) AJ, 106, p. 1059
  • Somers, G., Pinsonneault, M.H., (2015) ApJ, 807, p. 174
  • Song, I., Bessell, M.S., Zuckerman, B., (2002) ApJ, 581, p. L43
  • Song, I., Zuckerman, B., Bessell, M.S., (2003) ApJ, 599, p. 342
  • Thomas, H.-C., Beuermann, K., Reinsch, K., (1998) A&A, 335, p. 467
  • Tokovinin, A., (2014) AJ, 147, p. 86
  • Torres, C.A.O., Quast, G.R., Da Silva, L., (2006) A&A, 460, p. 695
  • Zacharias, N., Urban, S.E., Zacharias, M.I., (2004) AJ, 127, p. 3043
  • Zacharias, N., Finch, C.T., Girard, T.M., (2013) AJ, 145, p. 44
  • Zapatero Osorio, M.R., Béjar, V.J.S., Pavlenko, Y., (2002) A&A, 384, p. 937
  • Zuckerman, B., Song, I., (2004) ARA&A, 42, p. 685

Citas:

---------- APA ----------
Messina, S., Santallo, R., Tan, T.G., Elliott, P., Feiden, G.A., Buccino, A., Mauas, P.,..., Jofré, E. (2017) . Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association. Astronomy and Astrophysics, 601.
http://dx.doi.org/10.1051/0004-6361/201628514
---------- CHICAGO ----------
Messina, S., Santallo, R., Tan, T.G., Elliott, P., Feiden, G.A., Buccino, A., et al. "Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association" . Astronomy and Astrophysics 601 (2017).
http://dx.doi.org/10.1051/0004-6361/201628514
---------- MLA ----------
Messina, S., Santallo, R., Tan, T.G., Elliott, P., Feiden, G.A., Buccino, A., et al. "Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association" . Astronomy and Astrophysics, vol. 601, 2017.
http://dx.doi.org/10.1051/0004-6361/201628514
---------- VANCOUVER ----------
Messina, S., Santallo, R., Tan, T.G., Elliott, P., Feiden, G.A., Buccino, A., et al. Age of the magnetically active WW Psa and TX Psa members of the β Pictoris association. Astron. Astrophys. 2017;601.
http://dx.doi.org/10.1051/0004-6361/201628514