UK APAP Network
Lead Research Organisation:
University of Strathclyde
Department Name: Physics
Abstract
Plasmas permeate our Universe, being present in stellar atmospheres, interstellar gas clouds in galaxies, planetary nebulae, supernova remnants, black hole accretion disks, and so on.
Spectroscopy of all these objects has shown a richness of information, in
particular in the spectral lines that are emitted by the ions that are present in the plasmas.
In recent years, an overwhelming amount of XUV spectroscopic data have been
obtained from the satellite missions such as SOHO, Hinode, STEREO, SDO, IRIS (solar) and Chandra, XMM-Newton, HST, FUSE
(non-solar), while upcoming and future missions such as Solar Orbiter will provide no let-up.
The state of matter in each object --- the distribution of temperature and density, chemical composition --- can be determined through diagnostic analysis of spectral data in which models, incorporating the full physics of the object, confront the observations.
In addition, seismology of stellar interiors, including our sun, are a unique probe of their structure.
Spectroscopy and seismology information are fundamental for our understanding of the origin and evolution of the Universe.
Collisions of electrons and photons with atoms, ions and molecules play a fundamental role in
characterizing astrophysical plasmas, and it is therefore necessary that accurate atomic data are calculated.
It might be surprising, but a large fraction of the spectra produced by ions is still unexplored.
Large discrepancies between observations and theory are also still present.
In recent years, we have shown the need to perform accurate calculations of
electron-ion collisions for individual ions, in order to solve the large, long-standing
discrepancies between observed and calculated line intensities in collisional (astrophysical and laboratory) plasmas.
Furthermore, there is also a long standing problem concerning the elemental abundance of our sun.
It is thought to be due to our incomplete understanding of how low light emerges from deep in its interior.
We propose calculations which will enable the interpretation of spectral
data from satellites and stellar seismology which will further our understanding of the solar corona, stellar atmospheres,
supernova remnants, nebulae and stars.
With this proposal, we aim to strengthen the collaboration between
experimental, observational and theoretical research. Our work will also impact upon the magnetic fusion
program and its quest for a safe, reliable and environmentally friendly energy source.
Spectroscopy of all these objects has shown a richness of information, in
particular in the spectral lines that are emitted by the ions that are present in the plasmas.
In recent years, an overwhelming amount of XUV spectroscopic data have been
obtained from the satellite missions such as SOHO, Hinode, STEREO, SDO, IRIS (solar) and Chandra, XMM-Newton, HST, FUSE
(non-solar), while upcoming and future missions such as Solar Orbiter will provide no let-up.
The state of matter in each object --- the distribution of temperature and density, chemical composition --- can be determined through diagnostic analysis of spectral data in which models, incorporating the full physics of the object, confront the observations.
In addition, seismology of stellar interiors, including our sun, are a unique probe of their structure.
Spectroscopy and seismology information are fundamental for our understanding of the origin and evolution of the Universe.
Collisions of electrons and photons with atoms, ions and molecules play a fundamental role in
characterizing astrophysical plasmas, and it is therefore necessary that accurate atomic data are calculated.
It might be surprising, but a large fraction of the spectra produced by ions is still unexplored.
Large discrepancies between observations and theory are also still present.
In recent years, we have shown the need to perform accurate calculations of
electron-ion collisions for individual ions, in order to solve the large, long-standing
discrepancies between observed and calculated line intensities in collisional (astrophysical and laboratory) plasmas.
Furthermore, there is also a long standing problem concerning the elemental abundance of our sun.
It is thought to be due to our incomplete understanding of how low light emerges from deep in its interior.
We propose calculations which will enable the interpretation of spectral
data from satellites and stellar seismology which will further our understanding of the solar corona, stellar atmospheres,
supernova remnants, nebulae and stars.
With this proposal, we aim to strengthen the collaboration between
experimental, observational and theoretical research. Our work will also impact upon the magnetic fusion
program and its quest for a safe, reliable and environmentally friendly energy source.
Planned Impact
The International effort to develop magnetic fusion as a safe, reliable and
environmentally friendly source of energy will be a key beneficiary of this work.
Magnetic fusion laboratories around the world (including JET/Culham in the UK) and especially the flagship
ITER program at Cadarache in France, make use of spectroscopic diagnostics to maximize their
control of the plasma.
The electron collision atomic data that we produce are and will be incorporated into the main fusion
modelling package (ADAS) used by these laboratories.
ADAS was and is developed and maintained by researchers at the University of Strathclyde.
The wide distribution of our basic atomic data in all major atomic databases means that
our data are also used by a wide range of laboratories and industries.
environmentally friendly source of energy will be a key beneficiary of this work.
Magnetic fusion laboratories around the world (including JET/Culham in the UK) and especially the flagship
ITER program at Cadarache in France, make use of spectroscopic diagnostics to maximize their
control of the plasma.
The electron collision atomic data that we produce are and will be incorporated into the main fusion
modelling package (ADAS) used by these laboratories.
ADAS was and is developed and maintained by researchers at the University of Strathclyde.
The wide distribution of our basic atomic data in all major atomic databases means that
our data are also used by a wide range of laboratories and industries.
People |
ORCID iD |
Nigel Badnell (Principal Investigator) |
Publications
Gu L
(2022)
X-ray spectra of the Fe-L complex III. Systematic uncertainties in atomic data
in Astronomy & Astrophysics
Badnell N
(2022)
H, He-like recombination spectra - IV. Clarification and refinement of methodology for l -changing collisions
in Monthly Notices of the Royal Astronomical Society
Wang Y
(2022)
Transient obscuration event captured in NGC 3227 II. Warm absorbers and obscuration events in archival XMM-Newton and NuSTAR observations
in Astronomy & Astrophysics
Dufresne R
(2021)
The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere
in Monthly Notices of the Royal Astronomical Society
Mao J
(2021)
R-matrix electron-impact excitation data for the O-like iso-electronic sequence
in Astronomy & Astrophysics
Description | Consolidated grant |
Amount | £458,051 (GBP) |
Funding ID | ST/R000743/1 |
Organisation | Science and Technologies Facilities Council (STFC) |
Sector | Public |
Country | United Kingdom |
Start | 03/2018 |
End | 03/2021 |
Title | CHIANTI - Atomic Database |
Description | CHIANTI is an atomic database developed by the Atomic Astrophysics research group at DAMTP, funded by STFC. It is now universally used by the solar physics community for the analysis of solar spectra, and is also widely used in the astrophysical community. Giulio Del Zanna is a key member of the CHIANTI team, and has led several CHIANTI papers and releases. |
Type Of Material | Improvements to research infrastructure |
Provided To Others? | Yes |
Impact | CHIANTI has facilitated the analysis of solar spectra leading to over 3350 citations. |
URL | http://www.chiantidatabase.org/ |
Description | Collaboration on CHIANTI atomic database |
Organisation | National Aeronautics and Space Administration (NASA) |
Department | Goddard Space Flight Center |
Country | United States |
Sector | Public |
PI Contribution | I have provided several major contributions in terms of atomic data software and documentation. The most recent one was CHIANTI version 10. We are now in 2023 preparing an update to the database. |
Collaborator Contribution | Everyone in the team contributes atomic data |
Impact | Over 3000 citations. CHIANTI is now the reference atomic database for astrophysics. |