This link has been bookmarked by 1 people . It was first bookmarked on 08 Aug 2008, by Marco Castellani.
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08 Aug 08
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for increasing the metallicity the ZAHB models tend to accumulate at the lower effective temperatures so that it decreases the range of masses predicted within the RR Lyrae instability strip
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Gaussian random distribution of masses
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flat random distribution of post-ZAHB evolutionary time.
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a straightforward application of pulsational results to HB evolutionary models predicts periods slightly larger than observed in well studied clusters like M 5 and M 3.
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On this basis only, one would conclude that the adopted pulsational theory gives the right width in temperature of the instability strip, but either the predicted strip is too cool, or the models are too luminous, if not a combination of both.
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current evolutionary HB models are indeed too luminous
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we decided to retain the already quoted theoretical framework, but calibrating the luminosity of the models to reproduce the period distribution as observed in M 3.
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RR Lyrae rich cases,
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