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We present the discovery of a very faint stellar system, SMASH 1, that is potentially a satellite of the Large Magellanic Cloud. Found within the Survey of the Magellanic Stellar History (SMASH), SMASH 1 is a compact ({r}h={9.1}-3.4+5.9 {pc}) and very low luminosity ({M}V=-1.0+/- 0.9, {L}V={10}2.3+/- 0.4 {L}ȯ ) stellar system that is revealed by

Data from solar line of sight velocity measurements are presented to demonstrate the existence of a synodic signal with a 6.5 m/sec amplitude. Recordings of alternate measurements of the resonantly scattered light intensity were made at 1 sec intervals and a mean ratio for the laboratory and solar lines was calculated over a 42 sec interval

Doppler velocity data are used to study solar cycle variation of the frequencies of solar acoustic oscillations from 1977 to 1988. The results show a clear shift in frequency of the cross-correlation peaks of -0.37 + or - 0.04 microHz peak to peak as the solar activity cycle progresses from maximum to minimum. This effect is dependent on the l

The signature of the Solar-Cycle appears clearly in the p-mode parameters (Jiménez-Reyes et al. 1998, Libbrecht & Woodard 1990, and Anguera et al. 1992). At present, the study of the p-mode parameter variation is a very active topic in helioseismology where, thanks to projects like BISON, IRIS, GONG, LOWL and MDI, we are able for the first time to

Clark and Park1 reported regions of enhanced variable emission at millimetre wavelengths on the solar disk. In this communication I compare mechanisms, and suggest a model for these sources.