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Editore: Dissertation.com, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: Phatpocket Limited, Waltham Abbey, HERTS, Regno Unito
Libro
Condizione: Like New. Used - Like New. Book is new and unread but may have minor shelf wear. Your purchase helps support Sri Lankan Children's Charity 'The Rainbow Centre'. Our donations to The Rainbow Centre have helped provide an education and a safe haven to hundreds of children who live in appalling conditions.
Editore: Dissertation.com, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: Lucky's Textbooks, Dallas, TX, U.S.A.
Libro
Condizione: New.
Editore: Dissertation.Com, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: Ria Christie Collections, Uxbridge, Regno Unito
Libro Print on Demand
Condizione: New. PRINT ON DEMAND Book; New; Fast Shipping from the UK. No. book.
Editore: Dissertation.com, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: THE SAINT BOOKSTORE, Southport, Regno Unito
Libro Print on Demand
Paperback / softback. Condizione: New. This item is printed on demand. New copy - Usually dispatched within 5-9 working days.
Editore: Dissertation.Com. - DO NOT USE 2003-10, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: Chiron Media, Wallingford, Regno Unito
Libro
PF. Condizione: New.
Editore: Dissertation.Com, 2003
ISBN 10: 1581122004ISBN 13: 9781581122008
Da: AHA-BUCH GmbH, Einbeck, Germania
Libro Print on Demand
Taschenbuch. Condizione: Neu. nach der Bestellung gedruckt Neuware - Printed after ordering - This dissertation describes work performed at the Palomar Testbed Interferometer (PTI) during 1998-2002. Using PTI, we developed a method to measure stellar angular diameters in the 1-3 milli-arcsecond range with a precision of better than 5%. Such diameter measurements were used to measure the mass-radius relations of several lower main sequence stars and hence verify model predictions for these stars. In addition, by measuring the changes in Cepheid angular diameters during the pulsational cycle and applying a Baade-Wesselink analysis we are able to derive the distances to two galactic Cepheids (h Aql & z Gem) with a precision of ~10%; such distance determinations provide an independent calibration of the Cepheid period-luminosity relations that underpin current estimates of cosmic distance scales. Second, we used PTI and the adaptive optics facility at the Keck Telescope on Mauna Kea to resolve the low mass binary systems BY Dra and GJ 569B, resulting in dynamical mass determinations for these systems. GJ 569B most likely contains at least one sub-stellar component, and as such represents the first dynamical mass determination of a brown dwarf. Finally, a new observing technique, dual star phase referencing, was developed and demonstrated at PTI. Phase referencing allows interferometric observations of stars previously too faint to observe, and is a prerequisite for large-scale interferometric astrometry programs such as the one planned for the Keck Interferometer; interferometric astrometry is a promising technique for the study of extra-solar planetary systems, particularly ones with long-period planets.