The Mass of the Classical Cepheid ADS 14859 Cycle 8

Details The Mass of the Classical Cepheid ADS 14859 Cycle 8 The Mass of the Classical Cepheid ADS 14859 Cycle 8

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8440e&link_type=abstract

HST Proposal ID #8440

Computer Science

Hst Proposal Id #8440

Scientific paper

The determination of accurate masses for Cepheid variable stars is required for quantitative understanding of these primary distance indicators, and also the related questions of the accuracy of evolutionary calculations and the role played by massive stars in galactic evolution. The system ADS 14859 = HR 8157 = V1334 Cyg provides a unique opportunity to determine a Cepheid mass because it has a visual binary orbit. The system consists of a wide pair {AB} discovered by Hough {1887}, and a newly discovered close system {Aa, b} which consists of the Cepheid {Aa} and a yet uncharacterized companion {Ab}. No mass information will be available, however, without the proposed HST FGS and STIS observations, particularly of the Ab star which cannot be observed from the ground. From the STIS observations we will determine the temperature and infer the mass of Ab. Combining this mass with the sum of all three masses of the system derived from the visual orbit and the mass of B from IUE observations provides the mass of the Cepheid {Aa}. In addition, the FGS observations {POS mode} of the Aa, b system can provide its inclination, and hence the sum of the two masses of that system, and ultimately the Cepheid mass. Furthermore, the short period system {Aa, b} should be resolvable with the improved FGS in TRANS mode. Thus, the combination of these observations will provide determinations of the Cepheid mass from both the close and wide orbits.

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