This illustration shows a star surrounded by a protoplanetary disk. Material from the thick disk flows along the star’s magnetic field lines and is deposited onto the star’s surface. When material hits the star, it lights up brightly. The star’s irregular illumination allows astronomers to measure the gap between the disk and the star by using a technique called “photo-reverberation” or “light echoes.” First, astronomers look at how much time it takes for light from the star to arrive at Earth. Then, they compare that with the time it takes for light from the star to bounce off the inner edge of the disk and then arrive at Earth. That time difference is used to measure distance, as the speed of light is constant. Credit: NASA/JPL-Caltech
For the 1st time, astronomers used echoes of light to determine the distance from a star to the inner wall of its surrounding planet-forming disk of dust and gas. “Understanding protoplanetary disks can help us understand some of the mysteries about exoplanets, the planets in solar systems outside our own,” said Huan Meng. “We want to know how planets form and why we find large planets called ‘hot Jupiters’ close to their stars.”
They used a method called “photo-reverberation,” also known as “light echoes.” When the central star brightens, some of the light hits the surrounding disk, causing a delayed “echo.” Scientists measured the time it took for light coming directly from the star to reach Earth, then waited for its echo to arrive. Thanks to Albert Einstein’s theory of special relativity, we know that light travels at a constant speed. To determine a given distance = speed of light x time light takes to get from one point to another.
To take advantage of this formula, scientists needed to find a star with variable emission, ie a star that emits radiation in an unpredictable, uneven manner. Our own sun has a fairly stable emission, but a variable star would have unique, detectable changes in radiation that could be used for picking up corresponding light echoes. Young stars, which have variable emission, are the best candidates. The star used in this study is YLW 16B, 400 light-years from Earth. YLW 16B has about the same mass as our sun, but at 1 million years old, it’s just a baby compared to our 4.6-billion-year-old home star.
Astronomers combined Spitzer data with observations from ground-based telescopes: the Mayall telescope at Kitt Peak National Observatory in Arizona, the SOAR and SMARTS telescopes in Chile, and the Harold L. Johnson telescope in Mexico. During 2 nights of observation, researchers saw consistent time lags between the stellar emissions and their echoes in the surrounding disk. The ground-based observatories detected the shorter-wavelength infrared light emitted directly from the star, and Spitzer observed the longer-wavelength infrared light from the disk’s echo. Because of thick interstellar clouds that block the view from Earth, astronomers could not use visible light to monitor the star.
Researchers then calculated how far this light must have traveled during that time lag: ~0.08 astronomical units, ie ~8% of the distance between Earth and its sun. This was slightly smaller than previous estimates with indirect techniques, but consistent with theoretical expectations. Although this method did not directly measure the height of the disk, researchers were able to determine that the inner edge is relatively thick.
Previously, astronomers have used the light echo technique to measure the size of accretion disks of material around supermassive black holes. Since no light escapes from a black hole, researchers compare light from the inner edge of the accretion disk to light from the outer edge to determine the disk size. This technique is also used to measure the distance to other features near the accretion disk, such as dust and the surrounding fast-moving gas.
While light echoes from supermassive black holes represent delays of days to weeks, scientists measured the light echo from the protoplanetary disk in this study to be a mere 74s. The approach can be applied to other systems of stars with planet-forming disks around them. “Knowing the exact position of the inner boundary of a protoplanetary disk is important to anyone who wants to understand planet evolution,” Meng says.
Most stars are born with a protoplanetary disk around them, and astronomers have known for a long time that there is a gap between the star and its disk because of 2 competing processes: Close to the star, its strong radiation ionizes gas particles in the disk, diverting them along the star’s magnetic field lines above and below the plane of the disk. The other mechanism that prevents the disk from reaching all the way to the star’s surface is heat. Once a dust particle gets too close to the star, it simply vaporizes and either falls onto the star or gets blown out of the system.
“The predominant one of those two mechanisms plays an important role in the evolution of the disk, and right now, we don’t know which it is,” Meng says. Until now, astronomers used a technique called interferometry to determine the position of the inner edge of protoplanetary disks, but that method requires assumptions about the shape of the disk, resulting in controversial findings. “Our method provides a completely independent measurement of which mechanism plays the predominant role now and in the future,” Meng says. http://www.eurekalert.org/pub_releases/2016-04/uoa-leg042516.php
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