EXPORT:: Near-IR observations of Vega-type and pre-main sequence stars

被引：40

作者：

Eiroa, C ^{[1
]}

Garzón, F

Alberdi, A

de Winter, D

Ferlet, R

Grady, CA

Cameron, A

Davies, JK

Deeg, HJ

Harris, AW

Horne, K

Merín, B

Miranda, LF

Montesinos, B

Mora, A

Oudmaijer, R

Palacios, J

Penny, A

Quirrenbach, A

Rauer, H

Schneider, J

Solano, E

Tsapras, Y

Wesselius, PR

机构：

[1] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain

[2] Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain

[3] Inst Astrofis Andalucia, E-18080 Granada, Spain

[4] TNO, TPD Space Instrumentat, NL-2600 AD Delft, Netherlands

[5] CNRS, Inst Astrophys, F-75014 Paris, France

[6] NASA, Goddard Space Flight Ctr, NOAO, STIS, Greenbelt, MD 20771 USA

[7] Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland

[8] Joint Astron Ctr, Hilo, HI 96720 USA

[9] DLR, Dept Planetary Explorat, D-12489 Berlin, Germany

[10] VILSPA, LAEFF, Madrid 28080, Spain

[11] Univ Leeds, Dept Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[12] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England

[13] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, La Jolla, CA 92093 USA

[14] Observ Paris, F-92195 Meudon, France

[15] Univ Complex Zernike, SRON, NL-9700 AV Groningen, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2001年 / 365卷 / 02期

关键词：

stars; emission-line; Be; stars : pre-main sequence; stars : variable : general; infrared : stars;

D O I：

10.1051/0004-6361:20000029

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present near-IR JHK photometric data of a sample of 58 main-sequence, mainly Vega-type, and pre-main sequence stars. The data were taken during four observing runs ill the period May 1998 to January 1999 and form part of a coordinated effort with simultaneous optical spectroscopy and photo-polarimetry. The near-IR colors of the MS stars correspond in most cases to photospheric colors, although noticeable reddening is present towards a fen objects, and these stars show no brightness variability within the observational errors. On the other hand, the PMS stars show near-IR excesses and variability consistent with previous data.

引用

页码：110 / 114

页数：5

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