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WDPlanets

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Planetary systems around white dwarfs

In the 25 years since the discovery of 51 Peg b, we went from not knowing if the Solar system is a fluke of Nature to realising that it is totally normal for stars to have planets. The common fate of practically all planet hosts i... ver más

30/09/2026

UNIVERSITY OF WARW...

3M€

Presupuesto del proyecto: 3M€

Líder del proyecto

UNIVERSITY OF WARWICK No se ha especificado una descripción o un objeto social para esta compañía.

TRL 4-5

Ver 2 Participantes

Financiación concedida El organismo H2020 notifico la concesión del proyecto el día 2021-06-13

Línea de financiación objetivo El proyecto se financió a través de la siguiente ayuda:

ERC-2020-ADG: ERC ADVANCED GRANT

I+D

Cerrada hace 4 años

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2 Participantes

UNIVERSITY OF WARWICK

2.54M€ | Lider

ELKEID

350.25K€ | Participante

Últimas noticias

29-11-2024: IDAE En las últimas 48 horas el Organismo IDAE ha otorgado 4 concesiones

29-11-2024: ECE En las últimas 48 horas el Organismo ECE ha otorgado 2 concesiones

29-11-2024: CMVAMADRID En las últimas 48 horas el Organismo CMVAMADRID ha otorgado 37 concesiones

Duración del proyecto: 63 meses Fecha Inicio: 2021-06-13
Fecha Fin: 2026-09-30

Líder del proyecto

UNIVERSITY OF WARWICK

TRL 4-5

Presupuesto del proyecto 3M€

Descripción del proyecto In the 25 years since the discovery of 51 Peg b, we went from not knowing if the Solar system is a fluke of Nature to realising that it is totally normal for stars to have planets. The common fate of practically all planet hosts is that they will eventually evolve into white dwarfs, the Earth-sized embers that are the evolutionary end-points of most stars. Many of the known planets will survive the post main-sequence evolution of their host stars - in the solar system, this includes Mars, and all planetary bodies beyond it. Firm evidence for evolved planetary systems at white dwarfs is found in the form of photospheric contamination from the accretion of planetary material, transits caused by clouds of debris, spectroscopic variability from planetesimals on ultra-short period orbits, and one volatile-rich gaseous disc formed from the evaporated atmosphere of a giant planet. These evolved planetary systems provide insight into the formation, structure, evolution, and ultimate fate of planets that are entirely complementary to, and in large parts unattainable by, the analyses of exo-planets orbiting main-sequence stars. Within this project, we will make use of the astrometric, spectroscopic and photometric observations from Gaia, DESI, WEAVE, SDSS-V and ZTF-II to carry out an ambitious and comprehensive research program of white dwarfs hosting remnants of planetary systems. (1) We will measure the bulk abundances of at least 1000 planetesimals from the spectroscopic analysis of newly discovered white dwarfs that are strongly contaminated by the accretion of planetary material, assembling detailed statistics of the composition of planetary building blocks and/or fragments. (2) We will identify dozens of minor and major planets in close orbits around white dwarfs, and we will characterise their physical and orbital properties. The combined results of both areas of research will greatly improve our understanding of the formation, structure, and evolution of planets.

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