Why Hot Horizontal Branch Stars Can Appear Redder Than Red Giants

Details Why Hot Horizontal Branch Stars Can Appear Redder Than Red Giants Why Hot Horizontal Branch Stars Can Appear Redder Than Red Giants

2003-05-23

arxiv.org/abs/astro-ph/0305461v1

Astron.Astrophys. 407 (2003) 303-310

Astronomy and Astrophysics

Astrophysics

7 pages, 6 figures, Astronomy and Astrophysic, accepted May 15 2003

Scientific paper

10.1051/0004-6361:20030827

In this paper we report on a curious feature in the V, (U-B) color-magnitude diagrams of globular clusters. In our database, we find that a considerable fraction of blue horizontal branch stars, hotter than the instability strip and cooler than the Grundahl et al. (1999) jump (i.e., 6000 <~ T_eff K <~ 10000), have (U-B) colors redder than their red giant progenitors. This red incursion is not expected on theoretical grounds, as horizontal branch stars (whose convective regions are less extended than in red giant structures) should not ``appear'' cooler than a red giant. Analyzing data from different telescopes we show that: 1) the horizontal branch red incursion is strongly dependent on the shape of the adopted U filter and to a lesser extent, on the B filter; 2) the photometry done with U filters which do not encompass the Balmer jump, do not show the blue horizontal branch red incursion; 3) the occurrence of this feature is also due to the peculiar dependence of the U and B magnitudes on stars effective temperature, gravity, and metallicity; 4) theoretical tracks can reproduce the observed horizontal branch morphology, provided that the appropriate (i.e. exactly responding to the filters effectively used in the observations) transmission curve efficiencies are used for deriving color-T_eff transformations; 5) the red incursion extent depends on metallicity.

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