Sun-Like Stars Emit Huge Superflares

The finding that Sun-like stars release superflares raises the possibility that the Sun might cause geomagentic storms on Earth.

AsianScientist (May 21, 2015) – A team of Japanese astronomers has used the High Dispersion Spectrograph on the Subaru Telescope to conduct spectroscopic observations of Sun-like “superflare” stars first observed and cataloged by the Kepler Space Telescope. The investigations, in the Publications of the Astronomical Society of Japan, focused on the detailed properties of these stars and confirmed that Sun-like stars with large starspots can experience superflares.

The team, made up of astronomers from Kyoto University, University of Hyogo, the National Astronomical Observatory of Japan (NAOJ) and Nagoya University, targeted a set of solar-type stars emitting very large flares that release total energies 10-10,000 times greater than the biggest solar flares.

Solar flares are energetic explosions in the solar atmosphere and are thought to occur by intense releases of magnetic energy around the sunspots. Large flares often cause massive bursts of high-speed plasma called coronal mass ejections (CMEs), which can lead to geomagnetic storms on Earth. Such storms can have severe impacts on our daily life by affecting systems such as communications and power grids.

This work follows up on earlier observations made in 2012, where the team reported finding several hundred superflares on solar-type stars by analyzing stellar observation data from Kepler Space Telescope.

This discovery was very important as it enabled the astronomers to conduct statistical analysis of superflares for the first time. However, more detailed observations were needed to investigate detailed properties of superflare stars and whether such massive flares can occur on ordinary single stars similar to our Sun.

Based on the initial discovery, the team carried out spectroscopic observations on 50 solar-type superflare stars selected from the Kepler Space Telescope’s data. From the investigation of the detailed properties of spectral lines, the team obtained several results.

More than half the observed 50 stars show no evidence of binarity (that is, they are not binary stars). The team confirmed the characteristics of the target stars as similar to those of the Sun.

On the basis of the Kepler data, superflare stars show somewhat regular, periodic changes in their brightness. The typical periods range from one day to a few tens of days. Such variations are explained by the rotation of the star and its starspots. It was found that the stars seem to become dimmer when their starspots are on their visible sides. Moreover, the timescales of the brightness variations should correspond to the stars’ rotation speeds.

Spectroscopic observations also allow observers to estimate the rotation velocity from the broadening of absorption lines and confirm that a velocity derived from spectroscopic data matches the brightness variation timescale as the star rotates. In addition, the measured rotation velocity of some target superflare stars is as slow as that of the Sun.

Based on solar observations, astronomers know that if there are large dark star spots on a stellar surface, the “core depth” (the depth and width of a spectral line) of the Ca II 854.2 nanometer (ionized Calcium) absorption line becomes shallow. Using this, they investigated the core depth of Ca II 854.2 nanometer line and found that superflare stars have large starspots compared to sunspots.

The results of these observations and analysis confirm that stars similar to the Sun can have superflares if they have large starspots. In the future, in addition to the continuing spectroscopic observations with Subaru Telescope, the team will conduct observations with the Kyoto University’s Okayama 3.8 meter telescope, which is now under construction. This will allow them to investigate more detailed properties and changes in the long-term activity of superflare stars.

The articles can be found at:
Notsu et al. (2015) High-dispersion Spectroscopy Of Solar-type Superflare Stars. I. Temperature, Surface Gravity, Metallicity And vsin i.
Notsu et al. (2015) High dispersion Spectroscopy Of Solar-type Superflare Stars. II. Stellar Rotation, Starspots And Chromospheric Activities.

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Source: Subaru Telescope, National Astronomical Observatory of Japan.
Disclaimer: This article does not necessarily reflect the views of AsianScientist or its staff.

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