Description
Hard X-ray emission from white dwarfs (WD) is generated by the presence of a stellar companion either by their coronal emission or by an accretion disk formed by the material stripped from the companion. Recent studies have proven that Jupiter-like planets can be the donors of material to create an accretion disk and generate hard X-ray emission. Under this light, here we discuss our X-ray XMM-Newton observations of the accreting WD G29-38 and the Central Star of the Helix Nebula. In addition, we present radiation-hydrodynamic simulations produced with the GUACHO code to study the WD+planet scenario. Synthetic X-ray observations are produced with the help of the CHIANTI database and are compared directly with observations.
Primary authors
Dr
Jesús Toalá
(IRyA-UNAM)
Dr
Martín Guerrero
(IAA)
Dr
Raúl F Maldonado
(IRyA-UNAM)
Sandino Estrada-Dorado
(Instituto de Ciencias Nucleares)
Dr
Verónica Lora
(ICN-UNAM)
Co-authors
Dr
J Alejandro Esquivel
(ICN-UNAM)
Dr
You-Hua Chu
