Megha, A.; Sampoorna, M.; Nagendra, K.N.; Anusha, L. S.; Sankarasubramanian, K.: Fast Iterative Techniques for Polarized Radiative Transfer in Spherically Symmetric Moving Media. The Astrophysical Journal 903 (1), 6 (2020)
Nagendra, K. N.; Sowmya, K.; Sampoorna, M.; Stenflo, J. O.; Anusha, L. S.: Importance of Angle-dependent Partial Frequency Redistribution in Hyperfine Structure Transitions Under the Incomplete Paschen–Back Effect Regime. The Astrophysical Journal 898 (1), 49 (2020)
Nagendra, K. N.; Sowmya, K.; Sampoorna, M.; Stenflo, J. O.; Anusha, L. S.: Importance of Angle-dependent Partial Frequency Redistribution in Hyperfine Structure Transitions Under the Incomplete Paschen-Back Effect Regime. The Astrophysical Journal 898, p. 49 (2020)
Anusha, L. S.: Solution of Multi-dimensional Polarized Radiative Transfer Equation with PFR. Radiative Signature from the Cosmos 519, pp. 105 - 108 (2019)
Megha, A.; Sampoorna, M.; Nagendra, K. N.; Anusha, L. S.; Sankarasubramanian, K.: Polarized Line Formation in Spherically Symmetric Atmospheres with Velocity Fields. The Astrophysical Journal 879 (1), 48 (2019)
Sampoorna, M.; Nagendra, K. N.; Sowmya, K.; Stenflo, J. O.; Anusha, L. S.: Polarized Line Formation in Arbitrary Strength Magnetic Fields: The Case of a Two-level Atom with Hyperfine Structure Splitting. The Astrophysical Journal 883 (2), 188 (2019)
Sampoorna, M.; Nagendra, K. N.; Sowmya, K.; Stenflo, J. O.; Anusha, L. S.: Polarized Line Formation in Arbitrary Strength Magnetic Fields: The Case of a Two-level Atom with Hyperfine Structure Splitting. The Astrophysical Journal 883, p. 188 (2019)
Anusha, L. S.; Sami, K. S.; Hirzberger, J.; Feller, A.: Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations. Astronomy and Astrophysics 598, A47 (2017)
Anusha, L. S.; Nagendra, K. N.; Uitenbroek, H.: Effect of Cross-Redistribution on the Resonance Scattering Polarization of O-I Line at 1302 Å. Astrophysical Journal 794 (1), 17 (2014)
Supriya, H. D.; Smitha, H. N.; Nagendra, K. N.; Stenflo, J. O.; Bianda, M.; Ramelli, R.; Ravindra, B.; Anusha, L. S.: Center-To-Limb Observations and Modeling of the Ca I 4227 Å Line. Astrophysical Journal 793 (1), 42 (2014)
Anusha, L. S.; Nagendra, K. N.: Multi-Dimensional Radiative Transfer to Analyze Hanle Effect In Ca II K line at 3933 Å. Astrophysical Journal 767 (2), 108 (2013)
Megha, A.; Sampoorna, M.; Nagendra, K. N.; Anusha, L. S.; Sankarasubramanian, K.: Resonance Line Polarization in Spherically Symmetric Moving Media: a Parametric Study. In: Proceedings of the 9th Solar Polarization Workshop SPW9 (Eds. Gandorfer, A. M.; Lagg, A.; Raab, K.). (2019)
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.
The Solar Lower Atmosphere and Magnetism (SLAM) group covers many exciting subjects in solar physics, focussing on the development and testing of highly novel solar instrumentation, reduction and analysis of highest quality solar observations, or improving and developing advanced techniques for the analysis of solar observations.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.
The Solar Lower Atmosphere and Magnetism (SLAM) group covers many exciting subjects in solar physics, focussing on the development and testing of highly novel solar instrumentation, reduction and analysis of highest quality solar observations, or improving and developing advanced techniques for the analysis of solar observations.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.