Background is Nova Cygni 1992 taken October 1996 with the FLWO 1.2m

I am a professor of Physics at the The University of Notre Dame. My research interests include cosmology, supernovae, cataclysmic variables, binary stars and GRB . My vita and list of publications.
The site is underconstruction

Supernovae and Cosmology

My research includes the study of supernovae and their use as cosmological probes. I was a member of the High-Z Supernova Search Team that used type Ia supernovae to show that the universal expansion is accelerating due to a mysterious dark energy. Supernova Hubble Diagram

Pictures of Cataclysmic Variables and Binary Stars:

RXJ 0558.0+5353 is a DQ Her type CV with an orbital period just over 4 hours and a white dwarf spin period of about 9 minutes. MMT spectra covering nearly an entire orbit were used to construct a Doppler tomograph of the HeII emission. A Doppler tomograph uses the spectral line shapes and orbital velocity variations to reconstruct an image of the accretion disk. The distribution of the emission in RXJ0558 is rather odd and probably results from both the impact of an accretion stream and heating by X-rays from the spinning white dwarf.

Nova Cygni 1992 (V1974 Cyg) exploded in February 1992. In 1996 a new emission nebula was discovered to the south of the nova. The nebula is apparently the result of light from the nova exciting interstellar gas nearby. It is likely that the nebula will expand with time as the light from the nova propagates further into the surrounding gas.

The light curve of the symbiotic nova PU Vul from AAVSO data shows an eclipse in 1995 corresponding to spectral variations monitored at DAO . Another eclipse was seen during the outburst in 1980 and proves that the orbital period of the binary is 13.4 years. Details can be found in the Garnavich (1996) Journal of the AAVSO , vol. 24, No. 2, p. 81.

Pictures of Jets from YSOs:

The region around S187 is filled with dark clouds and reflection nebulae. In the near-infrared we cut through the extinction and can see a number of jets in molecular hydrogen (2.12 microns). In images taken with the Fred Whipple Obs. 1.2m telescope, one jet appears bent and is either curved due to an outflow pushing from the north or the jet source is precessing.

The "snake" near LkHa234 in narrow band molecular hydrogen at 2.12 microns (red), off band at 2.22 microns (blue) and optical R band 0.67 microns (green). Images were obtained with the 3.5m telescope + GRIM-II at the Apache Point Observatory . The "snake" is really the edge of a dense cloud which is excited by UV radiation from nearby young stars.

The region near HH 110 (2-6) in narrow band molecular hydrogen emission at 2.12 microns. Two new jets (9-11 and 12-13) are visible only in the infrared. Details can be found in Garnavich, Noriega-Crespo, Raga and Bohm (1997), ApJ , 490, 752.

The bright jet Cepheus-E in narrow band molecular hydrogen emission at 2.12 microns. Images from the 3.5m APO telescope. An IR spectrum of the southern knot taken with the MMT and Rieke FSPEC spectrometer shows a very rich molecular hydrogen spectrum.

For more information, please contact Peter M. Garnavich