Researchers from Rice University believe that although stars dispersed throughout the sky appear distinct, they may actually be more similar than previously believed.
The sun and other “cool” stars share dynamic surface behaviors that affect their energy and magnetic surroundings, according to new modeling work by Rice scientists. If a star has planets that might harbor life, it depends on their stellar magnetic activity.
In a study that was published in The Astrophysical Journal, astrophysicists David Alexander and Christopher Johns-Krull collaborated with Rice postdoctoral researcher Alison Farrish.
In order to forecast how magnetic activity will effect any exoplanets in their systems, the research establishes a link between the rotation of cool stars and the behavior of their surface magnetic flux. This surface magnetic flux behavior drives the star’s coronal X-ray luminosity.
The research comes after another conducted by Farrish and Alexander that suggested a star’s “weather” in space might render planets in its “Goldilocks zone” inhospitable.
“All stars spin down over their lifetimes as they shed angular momentum, and they get less active as a result,” Farrish said. “We think the sun in the past was more active and that might have affected the early atmospheric chemistry of Earth. So thinking about how the higher energy emissions from stars change over long timescales is pretty important to exoplanet studies.”
“More broadly, we’re taking models that were developed for the sun and seeing how well they adapt to stars,” said Johns-Krull.
On the basis of the scant information available, the researchers set out to mimic what distant stars are like. Some stars’ spin and flux, as well as their classification types F, G, K, and M, which provided details on their sizes and temperatures, have been identified.
They compared the characteristics of the sun, a G-type star, with those of other cool stars by using its Rossby number, a measure of stellar activity that takes into account both the rotational speed and the subsurface fluid flows that affect the distribution of magnetic flux on a star’s surface. According to their models, the “space weather” of each star affects the conditions of its corresponding planets in a similar manner.
All stars like the sun fuse hydrogen and helium in their cores and that energy is first carried in the radiation of photons toward the surface. But it hits a zone about 60% to 70% of the way that’s just too opaque, so it starts to undergo convection. Hot matter moves from below, the energy radiates away, and the cooler matter falls back down.
Christopher Johns-Krull
“The study suggests that stars at least cool stars are not too dissimilar from each other,” Alexander said. “From our perspective, Alison’s model can be applied without fear or favor when we look at exoplanets around M or F or K stars, as well, of course, as other G stars.”
“It also suggests something much more interesting for established stellar physics, that the process by which a magnetic field is generated may be quite similar in all cool stars. That’s a bit of a surprise,” he said. This could include stars that, unlike the sun, are convective down to their cores.
“All stars like the sun fuse hydrogen and helium in their cores and that energy is first carried in the radiation of photons toward the surface,” Johns-Krull said. “But it hits a zone about 60% to 70% of the way that’s just too opaque, so it starts to undergo convection. Hot matter moves from below, the energy radiates away, and the cooler matter falls back down.”
“But stars with less than a third of the mass of the sun don’t have a radiative zone; they’re convective everywhere,” he said. “A lot of ideas about how stars generate a magnetic field rely on there being a boundary between the radiative and the convection zones, so you would expect stars that don’t have that boundary to behave differently. This paper shows that in many ways, they behave just like the sun, once you adjust for their own peculiarities.”
The model only applies to unsaturated stars, according to Farrish, who recently received her doctorate from Rice and will shortly undertake a postdoctoral research position at NASA’s Goddard Space Flight Center.
“The most magnetically active stars are the ones we call ‘saturated,’” Farrish said. “At a certain point, an increase in magnetic activity stops showing the associated increase in high energy X-ray emission. The reason that dumping more magnetism onto the star’s surface doesn’t give you more emission is still a mystery.”
“Conversely, the sun is in the unsaturated regime, where we do see a correlation between magnetic activity and energetic emission,” she said. “That happens at a more moderate activity level, and those stars are of interest because they might provide more hospitable environments for planets.”
“The bottom line is the observations, which span four spectral types including both fully and partially convective stars, can be reasonably well represented by a model generated from the sun,” Alexander said. “It also reinforces the idea that even though a star that is 30 times more active than the sun may not be a G-class star, it’s still captured by the analysis that Alison has done.”
“We do have to be clear that we’re not simulating any specific star or system,” he said. “We are saying that statistically, the magnetic behavior of a typical M star with a typical Rossby number behaves in a similar fashion to that of the sun which allows us to assess its potential impact on its planets.”
The star’s activity cycle is a crucial unknown that must be accounted for in the models through years of observation. (The sun’s cycle is 11 years, evidenced by sunspot activity when its magnetic field lines are most distorted.)
Johns-Krull said the model will still be useful in many ways. “One of my areas of interest is studying very young stars, many of which are, like low-mass stars, fully convective,” he said. “Many of these have disc material around them and are still forming planets. How they interact is mediated, we think, by the stellar magnetic field.”
“So, Alison’s modeling work can be used to learn about the large-scale structure of very magnetically active stars, and that can then allow us to test some ideas about how these young stars and their disks interact.”
Minjing Li, a visiting undergraduate from the University of Science and Technology of China, is a co-author of the paper. Alexander is a professor of physics and astronomy and director of the Rice Space Institute. Johns-Krull is a professor of physics and astronomy.
A National Science Foundation INSPIRE grant supported the research.
