February 1, 2012
‘Cool’ Gas May Form And Strengthen Sunspots
Hydrogen molecules may act as a kind of energy sink that strengthens the magnetic grip that causes sunspots, according to scientists from Hawaii and New Mexico using a new infrared instrument on an old telescope.
"We think that molecular hydrogen plays an important role in the formation and evolution of sunspots," said Dr. Sarah Jaeggli, a recent University of Hawaii at Manoa graduate whose doctoral research formed a key element of the new findings. She conducted the research with Drs. Haosheng Lin, also from the University of Hawaii at Manoa, and Han Uitenbroek of the National Solar Observatory in Sunspot, NM. Jaeggli now is a postdoctoral researcher in the solar group at Montana State University. Their work is published in the Feb. 1, 2012, issue of The Astrophysical Journal.They used the new Facility Infrared Spectropolarimeter (FIRS) at the Dunn Solar Telescope at Sunspot, NM, and the older Horizontal Spectrograph. Although built in 1969, the Dunn now is equipped with advanced adaptive optics that correct for much of atmospheric blurring.
The team analyzed seven active regions on the Sun, one in 2001 and six during December 2010 to December 2011 as Sunspot Cycle 23 faded away. The full sunspot sample has 56 observations of 23 different active regions.
Sunspots appear to come and go in approximate 11-year cycles. They are brighter than an arc-welder's torch, but appear black because the surrounding solar surface is so much brighter. Galileo and his contemporaries discovered sunspots in 1610. George Ellery Hale discovered magnetism in spots in 1908, and scientists soon determined that intense magnetism suppresses the normal convective motions present throughout the solar photosphere and forms "cool" spots.
But the details remain a mystery. Among the clues solar physicists have observed is a direct relationship between the spot's inner temperature and its magnetic field strength. But at very low temperatures, the field strength makes a sharp rise.
"This result is puzzling," Jaeggli and her colleagues wrote. It implies some undiscovered mechanism inside the spot.
One suspect is hydrogen atoms combining into hydrogen molecules (H2). The Sun is about 90 percent hydrogen atoms (plus 10 percent helium and 0.13 percent everything else). Most of the hydrogen is ionized atoms since the average surface temperature is an inferno-like 5780K (9944 deg. F). Yet it is a "cool star" since astronomers can detect heavy-element molecules in the solar spectrum. In 1997 they even found water, as traces of super-heated steam, inside spots.
This suggests that a spot's cool umbra, the "black" shadow at center, might let hydrogen molecules combine in surface layers. As early as 1986 the late Prof. Per E. Maltby and colleagues at the University of Oslo predicted that the gas in the umbra could be as much as 5 percent hydrogen molecules.
Such a shift would cause a major change in sunspot dynamics. A basic law of physics is that gas particles exert the same pressure whether they are atoms or molecules. A hydrogen molecule will provide half the pressure of the two atoms it used to be. And bonds between atoms oscillate and rotate, thus storing energy without raising the temperature. (This is why water absorbs a lot of heat before boiling.)
"The formation of a large fraction of molecules may have important effects on the thermodynamic properties of the solar atmosphere and the physics of sunspots," Jaeggli wrote.
But direct measurement of hydrogen molecules in spots is beyond our grasp for now, so the team measured a stand-in, the hydroxyl radical made of one atom each of hydrogen and oxygen (OH). About 1 percent of the mass of the Sun is oxygen. OH dissociates (breaks into atoms) at a slightly lower temperature than H2, meaning H2 can also form in regions where OH is present. By coincidence, one of its infrared spectral lines is 1565.2nm, almost the same as the 1565nm line of iron, used for measuring magnetism in a spot and one of the lines FIRS is designed to observe. (These are twice the wavelength of the deepest red, 770nm, the human eye can see.)
First using the older HSG in 2001, and then with the more advanced FIRS in 2009-10, the team measured magnetic fields across sunspots, and the OH intensity inside spots. From that, they calculated the H2 concentrations.
"We found evidence that significant quantities of hydrogen molecules form in sunspots that are able to maintain magnetic fields stronger than 2,500 Gauss," Jaeggli said. By comparison, Earth's magnetic field, which turns a compass needle, is about one-half Gauss. The team estimated a hydrogen molecule quantity of a few percent.
Jaeggli said its presence leads to a temporary "runaway" intensification of the magnetic field. Magnetic flux emerges from the interior and suppresses convection at the surface, trapping cool gas that has radiated its energy into space. Molecular hydrogen forms, reducing the volume. This is more transparent than atomic hydrogen, so more energy radiates into space, cooling the gas further. Hot gases around the emerging flux compress the cooler region and intensify the magnetic field.
Eventually it levels out, partly from energy radiating in from the surrounding gas. Otherwise, the spot would grow without bounds. As the magnetic field weakens, the H2 and OH molecules heat up and dissociate back to atoms, compressing the remaining cool regions and keeping the spot from collapsing.
The team says that simulations are needed to test their observations. They also note that most of the active regions observed are of modest field strength. They expect that Cycle 24, which is now ramping up, will provide stronger active regions for a test of their hypothesis.
NSO's mission is to advance knowledge of the Sun, both as an astronomical object and as the dominant external influence on Earth, by providing forefront observational opportunities to the research community. NSO is operated by Association of Universities for Research in Astronomy (AURA Inc.) under a cooperative agreement with the National Science Foundation (NSF) for the benefit of the astronomical community.
Founded in 1967, the Institute for Astronomy at the University of Hawaii at Manoa conducts research into galaxies, cosmology, stars, planets, and the Sun. Its faculty and staff are also involved in astronomy education, deep space missions, and in the development and management of the observatories on Haleakala and Mauna Kea.
Jaeggli, S. A.; Lin, H.; Uitenbroek, H. 2012. On Molecular Hydrogen Formation and the Magnetohydrostatic Equilibrium of Sunspots. The Astrophysical Journal, Feb. 1, 2012. 745 133 or arXiv:1110.0575v2.
Jaeggli, S. A. 2011. An Observational Study of the Formation and Evolution of Sunspots. Dissertation presentation, June 13, 2011. http://solar.physics.montana.edu/jaeggli/pubs.html
The Facility Infrared Spectropolarimeter (FIRS) at the National Solar Observatory's Dunn Solar Telescope is an advanced imaging spectropolarimeter developed by Haosheng Lin and colleagues at the Institute for Astronomy, University of Hawaii at Manoa, and NSO.
FIRS provides simultaneous spectral coverage at visible and infrared wavelengths through the use of a unique dual-armed spectrograph. The geometry of the spectrograph has been specially designed to capture 630.2nm and 1564.8nm lines of hot, neutral iron (Fe I) with maximum efficiency. It can be re-tuned so the infrared arm instead captures light from helium or silicon around 1083nm or, for this study, OH at 1565nm.
In addition, the spectrograph operates in a multiple slit mode. By using narrowband filters, the spectra from four consecutive slit positions can be imaged at once on the same detector. This feature decreases fourfold the time necessary to scan across a large area on the sun, making it an ideal instrument for the study of quickly developing active regions as illustrated in this "data cube" movie. It also operates simultaneously with other instruments at the Dunn, making for powerful observational capabilities.
More information is available at the FIRS web site. FIRS was supported by the National Science Foundation Major Research Program, Award No. ATM-0421582. (adapted from the FIRS web site).
Image 1: During the initial stage of sunspot emergence and cooling, the formation of H2 may trigger a temporary "runaway" magnetic field intensification. The magnetic field prevents the flow of energy from inside the sun to the outside, and the sunspot cools as the energy shines into space. They form hydrogen molecules that take half the volume of the atoms, thus dropping pressure and concentrating the magnetic field, and so on. (adapted from Jaeggli, 2011; sunspot image by F. Woeger et al)
Image 2: NOAA 11131 sunspot region (Dec. 6, 2010) was the most intense spot measured in this study, but far from the largest the Sun can produce. The two bottom images show the strength of the magnetic field (C) and the contrast between the interior of the spot and the surrounding photosphere (D). The first graph (A) shows how OH starts to appear in the penumbra and continues to rise as the magnetic field strength rises. Because OH forms at a lower temperature than H2, its presence implies the quantity of hydrogen molecules that could be present (B). (Adapted from Jaeggli et al, 2012)
Image 3: Spectral lines are the unique "fingerprints in light" that all atoms and molecules produce. In the presence of a magnetic field in a hot gas, some lines split, betraying the presence and strength of the magnetic fields. Each line corresponds to electrons giving up energy in discrete amounts, or quanta, as light. Imposing a magnetic field on the atom makes the electrons produce multiple lines instead of one. The spread of these lines is a direct measure of the strength of the magnetic field, and is greater in the red and then the infrared spectrum. This image depicts sunspot spectra taken by FIRS with lines centered at 630.2nm (left) and 1564.8nm (right). Note the broadened area in the color ellipses, indicating line splitting inside a spot, and how the broadening is greater at the longer wavelength. Contrast is adjusted to enhance visibility in the inset boxes. (Source: IfA, UH)
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