Kinich Pakal

Wed, 27 Apr 2016 00:00:00 +0000

The atmosphere of the Solar-like stars is composed of the photosphere, chromosphere, transition zone, and corona. The chromosphere is the layer where the temperature goes from 4000 K to 8000 K and is studied at ultraviolet, visible, infrared, millimeter and (sub)-millimeter wavelengths (Wedemeyer et al. 2016)¹. The first chromospheric models were obtained thanks to the ultraviolet observations (Vernazza et al. 1981; Avrett & Loeser 2008)² ³. However, recent observations made with the Solar Submillimeter Telescope (SST) and the Atacama Large Millimeter / Submillimeter Array (ALMA) have shown that the chromosphere has lower temperatures than expected by ultraviolet models (Linsky 2017). ⁴

We have developed the KINICH-PAKAL (Tapia-Vázquez, & De la Luz 2020)⁵ code that use the Levenberg-Marquard algorithm as a nonlinear fit method, PAKAL-MPI as a chromospheric model of the solar atmosphere, and observations at wavelengths ranging from infrared to millimeter to generate a more accurate model of the chromospheres of the solar-type stars. KINICH-PAKAL has allowed us to study in detail how the physical conditions of the atmosphere change as a function of its effective temperature. Developing these models is necessary for debris disk studies (White et al. 2018)⁶, study the conditions under which flares are formed (MacGregor et al.2018)⁷ and the possible physical mechanisms of flux variations in the stars (Liseau 2019)⁸.

References

Wedemeyer, S., Bastian, T., Brajša, R., et al. 2016, SSRv, 200, 1. ↩︎
Vernazza, J. E., Avrett, E. H., & Loeser, R. 1981, ApJS,45, 635. ↩︎
Avrett, E. H., & Loeser, R. 2008, ApJS, 175, 229. ↩︎
Linsky, J. L. 2017, ARA&A, 55, 159. ↩︎
Tapia-Vázquez, F., & De la Luz, V. 2020, ApJS, 246, 5. ↩︎
White, J.A., Aufdenberg, J., Boley, A.C., 2018, ApJ,859(2), p.102. ↩︎
MacGregor, M. A., Weinberger, A. J., Wilner, D. J., Kowalski, A. F., & Cranmer, S. R. 2018, ApJ, 855, L2. ↩︎
Liseau, R. 2019, arXiv:1904.03043. ↩︎

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Kinich Pakal

References