Are Planetary Nebulae and Proto-Planetary Nebulae Shaped by a Binary? Results of a Long-Term Radial Velocity Study

Details Are Planetary Nebulae and Proto-Planetary Nebulae Shaped by a Binary? Results of a Long-Term Radial Velocity Study Are Planetary Nebulae and Proto-Planetary Nebulae Shaped by a Binary? Results of a Long-Term Radial Velocity Study

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545421h&link_type=abstract

American Astronomical Society, AAS Meeting #215, #454.21; Bulletin of the American Astronomical Society, Vol. 42, p.471

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Planetary nebulae (PNs) and proto-PNs (PPNs) commonly reveal a bipolar or ellipsoidal nebula. The current working hypothesis is that this axial symmetry is caused by a binary companion. To test this hypothesis, we are carrying out a long-term radial velocity study of seven bright PPNs. They each have spectral types of F-G with many sharp lines that allow good precision (< 1 km/s). Initial observations made in 1991-1995 have been combined with our current observations from 2007-2009, all made with the 1.2-m Coude at the Dominion Astrophysical Observatory (DAO). In several cases, we have been able to include additional published radial velocities. All of the PPNs are found to vary within a full range of 10 km/s due to pulsation, with amplitudes of 2.0-2.5 km/s and periods of 35-130 days. Similar pulsation periods are found from our complementary light curve studies. Only one PPN, IRAS 22272+5435, shows evidence of additional velocity variation due to a binary. The resulting limits on possible binary companions to these PPNs will be presented. This research is funded in part by grants from the NSF.

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