Astronomers have come up with a new and improved method for measuring the masses of millions of solitary stars, especially those with planetary systems.
Getting accurate measurements of how much stars weigh not only plays a crucial role in understanding how stars are born, evolve and die, but it is also essential in assessing the true nature of the thousands of exoplanets now known to orbit most other stars.
The method is tailor-made for the , which is in the process of mapping the Milky Way galaxy in three dimensions, and , which is scheduled for launch next year and will survey the 200,000 brightest stars in the firmament looking for alien earths.
(Vanderbilt University)
鈥淲e have developed a novel method for 鈥榳eighing鈥� solitary stars,鈥� , who directed the development. 鈥淔irst, we use the total light from the star and its parallax to infer its diameter. Next, we analyze the way in which the light from the star flickers, which provides us with a measure of its surface gravity. Then we combine the two to get the star鈥檚 total mass.鈥�
Stassun and his colleagues鈥� in Italy, and 鈥攄escribe the method and demonstrate its accuracy using 675 stars of known mass in an article titled accepted for publication in the .
Traditionally, the most accurate method for determining the mass of distant stars is to measure the orbits of double star systems, called binaries. Newton鈥檚 laws of motion allow astronomers to calculate the masses of both stars by measuring their orbits with considerable accuracy. However, fewer than half of the star systems in the galaxy are binaries, and binaries make up only about one-fifth of red dwarf stars that have become prized hunting grounds for exoplanets, so astronomers have come up with a variety of other methods for estimating the masses of solitary stars. The photometric method that classifies stars by color and brightness is the most general, but it isn鈥檛 very accurate. Asteroseismology, which measures light fluctuations caused by sound pulses that travel through a star鈥檚 interior, is highly accurate but only works on several thousand of the closest, brightest stars.
鈥淥ur method can measure the mass of a large number of stars with an accuracy of 10 to 25 percent. In most cases, this is far more accurate than is possible with other available methods, and importantly it can be applied to solitary stars so we aren鈥檛 limited to binaries,鈥� Stassun said.
The technique is an extension of an approach that Stassun developed four years ago with graduate student , who is now an assistant professor at Pennsylvania State University. Using special of Vanderbilt astronomers, Bastein discovered a subtle flicker pattern in starlight that contains valuable information about a star鈥檚 surface gravity.
Last year, Stassun and his collaborators developed using published star catalog data. It involves combining information on a star鈥檚 luminosity and temperature with Gaia Mission parallax data. (The parallax effect is the apparent displacement of an object caused by a change in the observer鈥檚 point of view.)
鈥淏y putting together these two techniques, we have shown that we can estimate the mass of stars catalogued by NASA鈥檚 Kepler mission with an accuracy of about 25 percent and we estimate that it will provide an accuracy of about 10 percent for the types of stars that the TESS mission will be targeting,鈥� said Stassun.
Establishing the mass of a star that possesses a planetary system is a critical factor in determining the mass and size of the planets circling it. An error of 100 percent in the estimate of the mass of a star, which is typical using the photometric method, can result in an error of as much as 67 percent in calculating the mass of its planets. This is roughly equivalent to the difference between a Mercury and an Earth. So, it is extremely important in properly assessing the nature of all the alien worlds that astronomers have begun detecting in recent years.
The research was funded by PAARE grant AST-1358862 and the research and innovation program.