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University Communications
New Mexico State University
Las Cruces, New Mexico

May 27, 2003

Astronomers discover new method of estimated dwarf novae distances
By Karl Hill

Astronomers using the Fine Guidance Sensors of the Hubble Space
Telescope to study dwarf novae unexpectedly discovered a new method
of estimating the distances to these strange double-star systems,
using their orbital periods and outburst brightness. In the process
they learned that dwarf novae tend to be farther away and much
brighter than previously thought. 

"This sends everybody back to the drawing board," said New Mexico
State University astronomer Joni Johnson. "The models for dwarf novae
have to be adjusted."

The findings of Johnson and her collaborators from NMSU, the
University of California at Riverside, the University of Washington
and the University of Texas at Austin were reported May 26 to the
American Astronomical Society meeting in Nashville.

The researchers used the orbiting Hubble Space Telescope to directly
calculate the distances to six dwarf novae and determine the star
systems' brightness. Their original intention was to check the
accuracy of commonly used methods of estimating distances to dwarf
novae, but "along the way serendipity intervened," Johnson said.

The researchers not only found that dwarf novae estimates have been
off the mark. They also discovered a remarkably tight correlation
between the orbital period of a dwarf nova system and the system's
brightness during its occasional outbursts -- the longer it takes the
pair of stars to orbit each other, the brighter the outburst, Johnson
said. 

"What this means is that we now have a better method of estimating
the distances to these systems," she said. "If we know the orbital
period of the binary system, we can predict its true luminosity at
outburst and calculate the distance to the system."

Dwarf nova systems are a type of cataclysmic variable -- stars that
sometimes increase in brightness dramatically. They are binary
systems in which the primary, more massive star is a white dwarf -- a
star about the size of Earth but with the mass of the sun -- and the
secondary star is often a cool red dwarf. 

The two stars are locked in a tight orbit, so close to each other
that the powerful gravity of the white dwarf strips material away
from the red dwarf. This material swirls around the white dwarf in
what is known as an accretion disk. 

"At times the system becomes unstable and the accretion disk dumps a
lot of material onto the surface of the white dwarf," Johnson said.
"During these outbursts, the system gets anywhere from a few times
brighter to 250 times brighter."

The two stars in a dwarf nova are so close they orbit each other in a
matter of hours, compared with the month it takes the moon to orbit
Earth or the year it takes Earth to orbit the sun. Known orbital
periods range from 78 minutes to 48 hours, Johnson said.

A key to learning more about these systems is knowing how far away
they are, she said. Previous distance estimates have been based
primarily on comparing the light spectrum of the secondary star in a
dwarf nova to that of a standard star of the same type a known
distance away. 

For more accurate measurements, the astronomers used the Fine
Guidance Sensors on the HST to obtain high-precision parallaxes for
six dwarf novae, including RU Pegasi, WZ Sagittae and YZ Cancri. They
also examined existing data on four other similar objects. Parallaxes
provide a way to accurately calculate distances by observing an
object from two vantage points and measuring its shift against its
background -- the greater the shift, or parallax angle, the closer
the object is to the observer.

With these measurements in hand, the researchers could calculate the
brightness of the dwarf novae without having to make any assumptions.

"It immediately became obvious that the secondary stars were not
normal by any means," Johnson said. "They didn't have the normal
luminosity for a star of the measured temperature and in fact were
brighter than expected. So the distance measurements to dwarf nova
systems were often wrong." 

The serendipity came in the unexpected discovery of a tight
correlation between the orbital period of the binary stars and their
true luminosity when the system is in outburst, she said. This
correlation gives astronomers a new tool for measuring the distances
to dwarf novae that are too far away to measure by parallaxes.

Johnson's collaborators on the project are Tom Harrison of NMSU,
Steve Howell of UC-Riverside, Paula Szkody of the University of
Washington, and Barbara McArthur and Fritz Benedict of UT-Austin. The
project was funded by NASA's HST Guest Observer Program.

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