Press Release

Majority of Planetary Nebulae May Arise from Binary Systems

By SpaceRef Editor
January 10, 2004
Filed under , ,
Majority of Planetary Nebulae May Arise from Binary Systems
nebula

Near the end of its lifetime, a star like the Sun ejects its outer layers into
space, producing a hazy cloud of material called a planetary nebula. The complex
shapes and dazzling colors of planetary nebulae make them some of the most
popular objects in the night sky, for both amateur observing and scientific study.

New research suggests that many if not most of the stellar corpses at the
centers of these wildly varied cosmic objects have companion stars, a surprising
finding that will influence how astronomers explain their origins.

Astronomers used the Wisconsin-Indiana-Yale-NOAO 3.5-meter telescope at the
National Science Foundation’s Kitt Peak National Observatory to take radial
velocity measurements of 11 central stars of planetary nebulae (PNe), looking
for the telltale, repeatable wobble that indicates the presence of a companion’s
gravitational influence. This technique is also used to search for extrasolar
planets around nearby stars. Ten of the 11 central stars of the PNe in the
recent study showed clear evidence for radial velocity oscillations.

"If our current results are confirmed with further observations, we could be at
the start of a revolution in the study of the origin of planetary nebulae," says
Howard Bond of the Space Telescope Science Institute in Baltimore, the principal
investigator of the results presented today in Atlanta at the 203rd meeting of
the American Astronomical Society. "If these nebulae arise from binary stars, it
implies a very different origin for these systems than what most astronomers had
thought."

It might be expected that nebulae ejected from spherical stars would be
spherical, but many years of telescope observations show this not to be the
case. In fact, most PNe are either elliptical or have pronounced lobes, often
accompanied by jet-like structures.

There is general agreement that in order to eject gas with these observed
morphologies, single stars would have to rotate rather rapidly or have
reasonably strong magnetic fields, which themselves are the product of stellar
rotation. However, the stars that most commonly eject PNe are large, bloated
giants, indisposed to fast rotation.

"The most direct way to spin up these vast, fluffy stars is by the action of an
orbiting companion. In extreme cases, as a red giant star gradually increases in
size, it may actually swallow a companion star, which would then spiral down
inside the giant and eventually eject its outer layers," explains Orsola De
Marco, an astronomer at the American Museum of Natural History (AMNH) in New
York and the lead author of the publication reporting the first results of this
project. "Despite this, the mainstream astronomical view remains rooted in
single star theories for the evolution of planetary nebulae, supported by the
small percentage of planetary nebulae central stars that that were previously
known to be binaries. However, our new research threatens to turn this viewpoint
on its head."

Astronomers currently believe that the majority of stars — those that begin
with no more than eight times the mass of our Sun — end their lives by ejecting
a planetary nebula and becoming a cosmic ember called a white dwarf. However,
the new results from the WIYN telescope suggest that the story may be more
complicated, in that an interaction with a companion star may be required to
produce most planetary nebulae.

"We need more data to determine the exact periods of the binary central stars,
since this is the only way to be sure of their binarity and eliminate other
possible physical sources that could simulate the stellar wobble," De Marco
says. "We are reasonably sure that these variations are due to binarity, but
determination of their precise periods is the only way to be sure. We must also
increase the size of our sample."

Among the objects observed in this initial study are Abell 78, NGC 6891, NGC
6210, and IC 4593. The new radial velocity measurements were taken by the WIYN
Hydra spectrographic instrument.

A previously released Hubble Space Telescope image of NGC 6210 is available at:
http://hubblesite.org/newscenter/newsdesk/archive/releases/1998/36/image/a

Co-authors of this work are Dianne Harmer of the National Optical Astronomy
Observatory (NOAO) in Tucson, AZ, and Andrew Fleming of Michigan Technological
University in Houghton, MI, an NSF Research Experiences for Undergraduates (REU)
student at AMNH during the summer of 2003.

These results (Abstract 127.03 in the AAS meeting program) will be discussed in
an oral session that begins at 10:00 a.m. on Thursday, January 8, in Regency VI.
This research has been accepted for publication in the February 1, 2004, issue
of Astrophysical Journal Letters.

Images of other planetary nebulae taken by Kitt Peak telescopes are available in
the NOAO Image Gallery at:

http://www.noao.edu/image_gallery/planetary_nebulae.html
and
http://www.noao.edu/outreach/aop/observers/pn.html

The Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5-meter telescope is located at Kitt
Peak National Observatory, 55 miles southwest of Tucson, AZ. Kitt Peak National
Observatory is part of the National Optical Astronomy Observatory, which is
operated by the Association of Universities for Research in Astronomy (AURA),
Inc., under a cooperative agreement with the National Science Foundation (NSF).

SpaceRef staff editor.