The Physics of Wave Dynamics in the Solar Atmosphere
Lead Research Organisation:
University of Warwick
Department Name: Physics
Abstract
Abstract:
The atmosphere of the Sun above the visible surface (photosphere) is divided in several distinct layers that include the chromosphere, transition region and corona. These layers are highly dynamic with exchange of matter and energy. It is still not clear what maintains the atmospheric temperatures against radiative losses - the so called heating problem. It is believed that waves have an important role in delivering energy from surface convection into the atmosphere, and may also cause cool chromospheric material to be launched up into the corona (resembling observed spicules). Furthermore, waves are seen in structures at all temperatures and play a part in the cooling process of coronal plasma (oscillating rain). In this project, we shall examine the role of waves at the physical interface between hot (coronal) and cool (chromospheric) plasmas. It will involve a combination of theory, observations and numerical simulation. It will use codes developed at Warwick (Lare3D) and data from the solar satellites Hinode, IRIS and SDO along with data from the DKIST ground based telescope due to begin operation in 2019.
Potential impact:
Out understanding of wave coupling will further our understanding of the problem of how the solar atmosphere is heated. Large-amplitude oscillations will provide insight into solar flares and coronal mass ejections, which are sources of space weather.
Aims and objectives:
A combined observational and theoretical (numerical) approach to further our understanding of the physical conditions for wave coupling between the various layers of the solar atmosphere.
Novelty:
We will be using the improved facilities of the Warwick 3d MHD code Lare3D, which now included efficient thermal conduction and radiative losses to better model wave propagation in the solar chromosphere. We shall combine observations from AIA and IRIS to look for oscillatory signatures that span both chromosphere and corona, which will also be preparatory work for the DKIST observatory that will come online in 2019.
The atmosphere of the Sun above the visible surface (photosphere) is divided in several distinct layers that include the chromosphere, transition region and corona. These layers are highly dynamic with exchange of matter and energy. It is still not clear what maintains the atmospheric temperatures against radiative losses - the so called heating problem. It is believed that waves have an important role in delivering energy from surface convection into the atmosphere, and may also cause cool chromospheric material to be launched up into the corona (resembling observed spicules). Furthermore, waves are seen in structures at all temperatures and play a part in the cooling process of coronal plasma (oscillating rain). In this project, we shall examine the role of waves at the physical interface between hot (coronal) and cool (chromospheric) plasmas. It will involve a combination of theory, observations and numerical simulation. It will use codes developed at Warwick (Lare3D) and data from the solar satellites Hinode, IRIS and SDO along with data from the DKIST ground based telescope due to begin operation in 2019.
Potential impact:
Out understanding of wave coupling will further our understanding of the problem of how the solar atmosphere is heated. Large-amplitude oscillations will provide insight into solar flares and coronal mass ejections, which are sources of space weather.
Aims and objectives:
A combined observational and theoretical (numerical) approach to further our understanding of the physical conditions for wave coupling between the various layers of the solar atmosphere.
Novelty:
We will be using the improved facilities of the Warwick 3d MHD code Lare3D, which now included efficient thermal conduction and radiative losses to better model wave propagation in the solar chromosphere. We shall combine observations from AIA and IRIS to look for oscillatory signatures that span both chromosphere and corona, which will also be preparatory work for the DKIST observatory that will come online in 2019.
Organisations
People |
ORCID iD |
| Erwin Verwichte (Primary Supervisor) | |
| Simon White (Student) |
Studentship Projects
| Project Reference | Relationship | Related To | Start | End | Student Name |
|---|---|---|---|---|---|
| ST/R505195/1 | 01/10/2017 | 30/09/2021 | |||
| 2108185 | Studentship | ST/R505195/1 | 01/10/2018 | 31/03/2022 | Simon White |
| ST/S505808/1 | 01/10/2018 | 10/12/2022 | |||
| 2108185 | Studentship | ST/S505808/1 | 01/10/2018 | 31/03/2022 | Simon White |