Summary
Stars with masses many times that of our Sun are the direct progenitors to cosmic phenomena such as supernova explosions, black holes, and gravitational wave (GW) sources.
Through electromagnetic observations we obtain empirical information of such massive stars, however decoding the radiation reaching us through our telescopes is a highly non-trivial exercise. To constrain fundamental properties like temperatures, radii, chemical abundances, and mass loss, the observed radiation is fit by means of model stellar atmospheres.
Observations and theory show that the radiation-dominated atmospheres of massive stars are highly complex, multi-dimensional systems. However, although 3D model atmospheres of sun-like stars have already been on the market for a while, for hot, massive stars we still rely solely on results derived from inadequate 1D simulations. This severely limits our knowledge of the basic physics of massive stars and our capacity to correctly interpret observations, thereby preventing progress also in the large number of astronomical fields (e.g., black hole and GW progenitor models) that rely on a firm understanding of the massive-star life-cycle. The time is now ripe to change this.
Building on the unique expertise of the PI and his team, in a groundbreaking effort we will here develop the very first 3D model atmospheres for hot, massive stars with winds. SUPERSTARS-3D will fundamentally improve our physical understanding of massive stars, and revolutionize analysis and interpretation of their observed radiation. By further confronting our pioneering simulations directly to state-of-the-art observations, we will derive unprecedented constraints on evolution and end-of-life models.
We will develop all new models in an open-source fashion and make them easily accessible for a broad community; as such, SUPERSTARS-3D will also provide the critical cornerstone from which a large number of future scientific programs undoubtedly will be built.
Through electromagnetic observations we obtain empirical information of such massive stars, however decoding the radiation reaching us through our telescopes is a highly non-trivial exercise. To constrain fundamental properties like temperatures, radii, chemical abundances, and mass loss, the observed radiation is fit by means of model stellar atmospheres.
Observations and theory show that the radiation-dominated atmospheres of massive stars are highly complex, multi-dimensional systems. However, although 3D model atmospheres of sun-like stars have already been on the market for a while, for hot, massive stars we still rely solely on results derived from inadequate 1D simulations. This severely limits our knowledge of the basic physics of massive stars and our capacity to correctly interpret observations, thereby preventing progress also in the large number of astronomical fields (e.g., black hole and GW progenitor models) that rely on a firm understanding of the massive-star life-cycle. The time is now ripe to change this.
Building on the unique expertise of the PI and his team, in a groundbreaking effort we will here develop the very first 3D model atmospheres for hot, massive stars with winds. SUPERSTARS-3D will fundamentally improve our physical understanding of massive stars, and revolutionize analysis and interpretation of their observed radiation. By further confronting our pioneering simulations directly to state-of-the-art observations, we will derive unprecedented constraints on evolution and end-of-life models.
We will develop all new models in an open-source fashion and make them easily accessible for a broad community; as such, SUPERSTARS-3D will also provide the critical cornerstone from which a large number of future scientific programs undoubtedly will be built.
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More information & hyperlinks
| Web resources: | https://cordis.europa.eu/project/id/101044048 |
| Start date: | 01-09-2022 |
| End date: | 31-08-2027 |
| Total budget - Public funding: | 1 995 750,00 Euro - 1 995 750,00 Euro |
Cordis data
Original description
Stars with masses many times that of our Sun are the direct progenitors to cosmic phenomena such as supernova explosions, black holes, and gravitational wave (GW) sources.Through electromagnetic observations we obtain empirical information of such massive stars, however decoding the radiation reaching us through our telescopes is a highly non-trivial exercise. To constrain fundamental properties like temperatures, radii, chemical abundances, and mass loss, the observed radiation is fit by means of model stellar atmospheres.
Observations and theory show that the radiation-dominated atmospheres of massive stars are highly complex, multi-dimensional systems. However, although 3D model atmospheres of sun-like stars have already been on the market for a while, for hot, massive stars we still rely solely on results derived from inadequate 1D simulations. This severely limits our knowledge of the basic physics of massive stars and our capacity to correctly interpret observations, thereby preventing progress also in the large number of astronomical fields (e.g., black hole and GW progenitor models) that rely on a firm understanding of the massive-star life-cycle. The time is now ripe to change this.
Building on the unique expertise of the PI and his team, in a groundbreaking effort we will here develop the very first 3D model atmospheres for hot, massive stars with winds. SUPERSTARS-3D will fundamentally improve our physical understanding of massive stars, and revolutionize analysis and interpretation of their observed radiation. By further confronting our pioneering simulations directly to state-of-the-art observations, we will derive unprecedented constraints on evolution and end-of-life models.
We will develop all new models in an open-source fashion and make them easily accessible for a broad community; as such, SUPERSTARS-3D will also provide the critical cornerstone from which a large number of future scientific programs undoubtedly will be built.
Status
SIGNEDCall topic
ERC-2021-COGUpdate Date
09-02-2023
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