[vsnet-campaign-orion 99] Eclipsing T Tau stars

[Taichi Kato]

Eclipsing T Tau stars

  According to the following astro-ph, RX J0529.4+0041 = V1642 Ori and
V1174 Ori are eclipsing T Tau(-like) stars.  Probably worth more regular
observation.

# RXJ0529+0041 = V1642 Ori
GSC101.1622 052920.61 +004127.8 (2000.0) 12.82 0
GSC101.1622 052920.64 +004128.1 (2000.0) 12.26 1
052919.5 +004122 (2000.0) 1RXPJ052919+0041.3 0.0131 0.00 0.00
052922.5 +004111 (2000.0) 1RXS_J052922.5+004112 0.052 0.63 0.39
052920.5 +004127 (2000.0) ORIV1642 E 12.30 13.07 V - - - -

# V1174 Ori
2MASS 053427.861 -054137.81 (2000.0) 11.241 10.610 10.389
053428.0 -054139 (2000.0) UBV_OrionB278 13.91 1.24 0.54 - - - - N=1 Nm=1 -
053427.7 -054137 (2000.0) ORIV1174 * INS: 15.6 16.7 P - - - R0/IBVS2565

Paper: astro-ph/0506767
Date: Thu, 30 Jun 2005 18:13:34 GMT   (96kb)

Title: What are the temperatures of T Tauri stars? - Constraints from coeval
  formation of young eclipsing binaries
Authors: M. Ammler (1), V. Joergens (2), R. Neuhaeuser (1) ((1)
  Astrophysikalisches Institut und Universitaetssternwarte Jena, (2)
  Sterrewacht Leiden)
Comments: accepted for publication in A&A, sect. 7 on 24/06/2005; 7 pages + 2
  appendices, 5 figures, 5 tables
\\
  We show how the assumption of coeval formation can be used to constrain the
effective temperatures of the components of young eclipsing double-lined
spectroscopic binaries. Our method extends the approach of White et al. (1999)
to a two-step analysis. The first step compares evolutionary models to the
observed masses and radii and selects those models that predict ages that are
consistent with coeval formation. The second step then uses these models to
constrain the effective temperatures. We applied the method on literature
values of the stellar parameters of the eclipsing binaries RX J0529.4+0041 A
and V1174 Ori and confirm that V1174 Ori A has dwarf-like temperatures at an
age of 9 Myrs, while we cannot draw any conclusions for RX J0529.4+0041 A and
V1174 Ori B. Considering these binaries, we find that none of the evolutionary
models gives coeval solutions simultaneously in mass, radius and effective
temperature.
\\ ( http://arXiv.org/abs/astro-ph/0506767 ,  96kb)