J/AcA/58/313 LMC Cepheids in OGLE and MACHO data (Poleski+, 2008)
Period changes of LMC Cepheids in the OGLE and MACHO data.
Poleski R.
<Acta Astron., 58, 313-328 (2008)>
=2008AcA....58..313P 2008AcA....58..313P
ADC_Keywords: Magellanic Clouds ; Stars, variable
Keywords: stars: oscillations - Cepheids - Magellanic Clouds
Abstract:
Pulsation period of Cepheids should change as stars evolve through the
instability strip. Rates of these changes found by other authors based
on the decades-long O−C diagrams show rather good agreement with
theoretical predictions. We have checked the variability on the scale
of a few years on the data recently published by the Optical
Gravitational Lensing Experiment (OGLE) for the Large Magellanic Cloud
Cepheids and found period changes for 18% of fundamental mode and 41%
of first overtone pulsators. It suggest the overtone pulsations are
less stable than the fundamental ones. For stars which had the
cross-references in the MACHO catalog we have checked if the period
change rates derived from the OGLE and the MACHO data are consistent.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 49 2946 List of all analyzed Cepheids
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See also:
J/AcA/58/163 : VI light curves of LMC classical Cepheids (Soszynski+, 2008)
ftp://ftp.astrouw.edu.pl/ogle/ogle3/OIII-CVS/lmc/cep/max_time : Home Page
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- --- [OGLE-LMC-CEP-]
14- 17 I04 --- Star Cepheid ID (OGLE LMC-CEP-NNNN)
19- 28 F10.7 d Per Mean pulsation period
30- 38 F9.7 d e_Per rms uncertainty on Per
40- 41 A2 --- Mode [F 1O] Pulsation mode (Fundamental or
1st overtone)
43- 49 A7 --- Rem Remarks (1)
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Note (1): Remarks as follows:
O = OGLE II data exist
V = MACHO V data exist
R = MACHO R data exist
A = amplitude is variable in at least one of the data sets
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History:
Copied at ftp://ftp.astrouw.edu.pl/ogle/ogle3/OIII-CVS/lmc/cep/max_time
(End) Patricia Vannier [CDS] 06-Apr-2010