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New Method Discovered for Estimating Distances to Dwarf Novae
27 May 2003
Nashville, TN --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 researchers from New Mexico State University, 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.

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diagram of tight binary

The researchers used the orbiting Hubble Space Telescope to directly calculate the distances to six dwarf novae and determine the star system's 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.

Collaborators on the project are Joni Johnson and 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.

Karl Hill
New Mexico State University
May 27, 2003

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13 August 2003
Astronomy Program · The University of Texas at Austin · Austin, Texas 78712
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