The UPS and Downs of Coordinated Observations

Details The UPS and Downs of Coordinated Observations The UPS and Downs of Coordinated Observations

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982msngr..29...12b&link_type=abstract

The Messenger, No.29, P. 12, 1982

Astronomy and Astrophysics

Astrophysics

Scientific paper

T Tauri stars are certainly not the only celestial objects for which coordinated observations are of interest. But their behaviour is sometimes so erratic that it is crucial to learn more about the range of the variations and about the correlations between variations in different wavelength domains than is allowed by one-telescope observations. Coordinated observations can overcome this limitation, but bring in their own problems. The question of the mass-flux in the envelopes of T Tauri stars can serve as a first example of how coordinated observations can help. By the end of the nineteen-fifties, it was accepted that T Tauri stars were newly-formed stars, still associated with the clouds from which they were born, and that they were losing mass. Observational evidence of mass-Ioss was confirmed when L. V. Kuhi derived, by modeling line profiles, mass-Ioss rates up to 6 . 10-7 M0 yr-1 . The belief that T Tauri stars had strong stellar winds went unchallenged until the late sixties, when M. F. Walker reported that a subclass of T Tauri stars, which he named YY Orionis stars, showed spectroscopic evidence for mass accretion. Our group at the Heidelberg Observatory studied active T Tauri stars extensively, and was able to show that a number of them were, at times, apparently accreting material. Even more confusing, Krautter and Bastian (1980, Astronomy and Astrophysics 88, L6) reported changes in the direction of the mass-f1ow on timeseales of days in DR Tauri, and even found evidence for simultaneous infall and outflow.

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