Variable winds on hot giant exoplanet help study of magnetic field

May 15, 2017
This image shows magnetic field lines in the atmosphere of a hot giant exoplanet. Time snapshot of magnetic field lines in the numerical simulation of a hot giant exoplanet atmosphere (a model of HD209458 b, but with a temperature structure similar to HAT-P-7 b). Magnetic field lines are colour-coded to represent the azimuthal (toroidal) magnetic field, with blue representing a negative-directed field (saturated at − 50 G) and magenta representing a positive-directed field (saturated at 50 G), with green and yellow ranging from − 5 to 5 G, respectively. The vantage point is looking onto the east-side terminator.

Senior Scientist Tamara M. Rogers of the Planetary Science Institute has discovered that substantial variability in the winds on the hot giant exoplanet HAT-P-7b are due to magnetism, and used those measurements to develop a new method to constrain the magnetic field of such an object.

HAT-P-7b was discovered by NASA's Kepler Mission in 2008. It is nearly 40 percent larger and nearly 80 percent more massive than Jupiter. It orbits its star every couple of days, and is so close that dayside temperature may be 2,200 degrees Kelvin (3,500 degrees Fahrenheit) with a night side 1,000 Kelvin (1,340 degrees Fahrenheit) cooler.

This strong day-night temperature difference drives strong eastward winds in the atmosphere and shifts the hottest temperature away from the point directly beneath the star on the dayside. However, this hot spot shifts significantly over time – even ending up on the west side of the sub-stellar point. This means that the winds are also changing significantly.

"The extreme temperatures of HAT-P-7b ionizes alkali metals such as lithium, sodium, and potassium, which results in the coupling of the atmosphere to a deep-seated magnetic field. Magnetic forces are able to then disrupt the strong eastward winds, leading to variable and even oppositely directed winds," Rogers said.

Rogers used a hydrodynamic model of the in combination with a magnetohydrodynamic (MHD) model to reproduce the observed variations in the hot spot location, thereby setting a minimum value for the strength of the magnetic field of this planet at six times that of the Earth.

"Long timeline or multiple epoch observations of hot giant phase curves coupled with MHD models of the atmospheres of these planets, can be used to place constraints on the magnetic field strengths of other hot giant exoplanets," Rogers said. "This will provide new insights into dynamo theory, planetary evolution and interpretations of star–planet magnetic interactions."

Rogers' paper "Constraints on the strengths of HAT-P-b and other hot giant exoplanets" appears in Nature Astronomy.

Explore further: The space weather forecast for Proxima Centauri B

More information: "Constraints on the Magnetic Field Strengths of HAT-P-b and Other Hot Giant Exoplanets," Tamara M. Rogers, 2017 May 15, Nature Astronomy www.nature.com/articles/s41550-017-0131 , Arxiv: arxiv.org/abs/1704.06271

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wduckss
1 / 5 (3) May 16, 2017
"Intermediate (andesitic) Temperatures: ~ 1000 ° C
Felsic (rhyolitic) Temp: <900 ° C
Magma is a complex high-temperature fluid substance. "https://en.wikipe...ki/Magma

"And is so close that daytime temperatures can be 2,200 degrees Kelvin (3,500 degrees Fahrenheit) with a night side 1,000 Kelvin (1,340 degrees Fahrenheit) cooler" from article

If it was not so, it confirms the planets from 100 to 740 AU of the stars and have the same temperature as HAT-P-7.
P third table
http://www.svemir...Universe
691Boat
not rated yet May 16, 2017
Considering the fact that HAT-P-7b is less dense than Jupiter (0.93 g/cm3 vs 1.33 g/cm3), not sure what magma has to do with anything. You make really goofy assumptions.
What are you actually trying to prove?

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