TY - JOUR
T1 - Generation of a circumstellar gas disc by hot Jupiter WASP-12b
AU - Debrecht, Alex
AU - Carroll-Nellenback, Jonathan
AU - Frank, Adam
AU - Fossati, Luca
AU - Blackman, Eric G.
AU - Dobbs-Dixon, Ian
N1 - Funding Information:
This work used the computational and visualization resources in the Center for Integrated Research Computing (CIRC) at the University of Rochester. Financial support for this project was provided by the Department of Energy grant GR523126, the National Science Foundation grant GR506177, and the Space Telescope Science Institute grant GR528562.
PY - 2018/8/1
Y1 - 2018/8/1
N2 - Observations of transiting extra-solar planets provide rich sources of data for probing the in-system environment. In the WASP-12 system, a broad depression in the usually bright Mg II h & k lines has been observed, in addition to atmospheric escape from the extremely hot Jupiter WASP-12b. It has been hypothesized that a translucent circumstellar cloud is formed by the outflow from the planet, causing the observed signatures.We perform 3D hydrodynamic simulations of the full system environment ofWASP-12, injecting a planetary wind and stellar wind from their respective surfaces.We find that a torus of density high enough to account for the lack of Mg II h & k line core emission in WASP-12 can be formed in approximately 13 yr. We also perform synthetic observations of the Lyman α spectrum at different points in the planet's orbit, which demonstrate that significant absorption occurs at all points in the orbit, not just during transits, as suggested by the observations.
AB - Observations of transiting extra-solar planets provide rich sources of data for probing the in-system environment. In the WASP-12 system, a broad depression in the usually bright Mg II h & k lines has been observed, in addition to atmospheric escape from the extremely hot Jupiter WASP-12b. It has been hypothesized that a translucent circumstellar cloud is formed by the outflow from the planet, causing the observed signatures.We perform 3D hydrodynamic simulations of the full system environment ofWASP-12, injecting a planetary wind and stellar wind from their respective surfaces.We find that a torus of density high enough to account for the lack of Mg II h & k line core emission in WASP-12 can be formed in approximately 13 yr. We also perform synthetic observations of the Lyman α spectrum at different points in the planet's orbit, which demonstrate that significant absorption occurs at all points in the orbit, not just during transits, as suggested by the observations.
KW - Hydrodynamics
KW - Planet-star interactions
KW - Planets and satellites: atmospheres
UR - http://www.scopus.com/inward/record.url?scp=85052430316&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85052430316&partnerID=8YFLogxK
U2 - 10.1093/MNRAS/STY1164
DO - 10.1093/MNRAS/STY1164
M3 - Article
AN - SCOPUS:85052430316
VL - 478
SP - 2592
EP - 2598
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -