A Sun more complex than expected

Figure 1: Visualization of the temperature structure across a vertical slice through a three-dimensional (3D) model of the solar atmosphere, taken from a state-of-the-art magneto-hydrodynamic simulation of the chromosphere-corona transition region (see Carlsson et al. 2016; A&A, 585, A4). The solid curve shows the heights (Z) in this model where the line-center photons of the hydrogen Lyman-α line observed by CLASP stem from (note that it practically delineates the model’s transition region). The investigat
Figure 1: Visualization of the temperature structure across a vertical slice through a three-dimensional (3D) model of the solar atmosphere, taken from a state-of-the-art magneto-hydrodynamic simulation of the chromosphere-corona transition region (see Ca
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Authors
Dr.
Javier Trujillo

The CLASP experiment (Chromospheric Lyman-Alpha Spectro-Polarimeter) was launched on 2015 September 3. The instrument, onboard a NASA suborbital rocket, measured with great success and for the first time the linear polarization of the strongest spectral line of the solar ultraviolet spectrum, the hydrogen Lyman-α line.

This international experiment (Japan, USA and Europe) was motivated by theoretical investigations carried out in 2011 at the Instituto de Astrofísica de Canarias (IAC). Thanks to the unprecedented observations provided by the CLASP instrument, the scientific team was able to confirm most of the theoretical predictions. However, the observed polarization signals, contrary to those calculated in today’s theoretical models of the solar atmosphere, do not show any significant variation in their line-center amplitude when the line of sight goes from the center to the edge of the solar disk. “This was a very interesting surprise that aroused great scientific interest, because the spectral lines of the solar visible spectrum (which can be observed with ground-based telescopes) show such a variation”, says Javier Trujillo Bueno, professor of the Spanish Research Council at the IAC and one of the principal investigators of CLASP.

The radiation of the Lyman-α line encodes information about the physical properties of the transition region, an enigmatic geometrically thin region where in less than 100 km the temperature suddenly jumps from the ten thousand degrees of the chromosphere to the million degrees of the corona. It is in these regions of the outer solar atmosphere where the explosive phenomena that can affect the Earth’s magnetosphere takes place. “The puzzling lack of a clear variation in the amplitude of the polarization signal when going from the center to the edge of the solar disk hides clues about the structure of the transition region”, says Jiri Stepan of the Astronomical Institute of the Academy of Sciences of the Czech Republic and one of the members of CLASP, presently on a working visit at the IAC.

The fact that the CLASP observations cannot be reproduced by today’s models of the solar atmosphere suggests that the 3D structure of the chromosphere-corona transition region is much more complex than previously thought.  In order to confirm this idea, the scientific team has carried out a complex theoretical investigation in order to determine the magnetization and geometrical complexity of the transition region that best explains the experimental data.

With the help of the MareNostrum supercomputer of the National Supercomputing Center in Barcelona, the researchers have calculated what would be the expected polarization signals for a large number of 3D atmospheric models, constructed by changing the degree of magnetization and geometrical complexity of the 3D solar model atmosphere illustrated in Figure 1.

Such study has led to two important conclusions, namely, the transition region of the atmospheric model that  most likely explains the CLASP observations has a significantly larger degree of geometrical complexity and a smaller degree of magnetization. The results of this investigation make it evident the need to develop more realistic 3D models of the solar atmosphere, by including phenomena such as spicules, ubiquitous in high-resolution observations of the line-core intensity in strong chromospheric lines (see Figure 2), but not present in today’s 3D models of the solar atmosphere.

More information in the article published in "The Astrophysical Journal Letters":

1.   Trujillo Bueno, J., Stepan, J., Belluzzi, L., et al. 2018, "CLASP Constraints on the Magnetization and Geometrical Complexity of the Chromosphere-Corona Transition Region", The Astrophysical Journal Letters, 866, L15

The Principal Investigators of the CLASP project are:

  • Amy Winebarger (NASA Marshall Space Flight Center, NASA/MSFC)
  • Ryouei Kano (National Astronomical Observatory of Japan, NAOJ)
  • Frédéric Auchère (Institut d'Astrophysique Spatiale, IAS)
  • Javier Trujillo Bueno (Instituto de Astrofísica de Canarias, IAC)

Related press releases:

Contacts at the IAC:

  • Javier Trujillo Bueno: jtb [at] iac.es (jtb[at]iac[dot]es)
  • Jiri Stepan: jiri.stepan [at] asu.cas.cz (jiri[dot]stepan[at]asu[dot]cas[dot]cz)
  • Andrés Asensio Ramos: aasensio [at] iac.es (aasensio[at]iac[dot]es)
  • Tanausú del Pino Alemán: tanausu [at] iac.es (tanausu[at]iac[dot]es)
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Astrophysics
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