Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b

P. Wilson Cauley, Seth Redfield, Adam G. Jensen, Travis Barman, Michael Endl, William D. Cochran

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

Hot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ∼70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ∼28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.

Original languageEnglish (US)
Pages (from-to)376-381
Number of pages6
JournalProceedings of the International Astronomical Union
Volume11
Issue numberS320
DOIs
StatePublished - Aug 1 2015

Fingerprint

bows
Jupiter (planet)
Jupiter
planets
stellar winds
planet
transit
shock
hydrogen
planetary magnetic fields
planetary magnetospheres
magnetosphere
field strength
outflow
time series
magnetic field
stars
orbitals
radii
high resolution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b. / Cauley, P. Wilson; Redfield, Seth; Jensen, Adam G.; Barman, Travis; Endl, Michael; Cochran, William D.

In: Proceedings of the International Astronomical Union, Vol. 11, No. S320, 01.08.2015, p. 376-381.

Research output: Contribution to journalArticle

Cauley, P. Wilson ; Redfield, Seth ; Jensen, Adam G. ; Barman, Travis ; Endl, Michael ; Cochran, William D. / Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b. In: Proceedings of the International Astronomical Union. 2015 ; Vol. 11, No. S320. pp. 376-381.
@article{fe173a25b5414c978b5e09276f12f1bd,
title = "Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b",
abstract = "Hot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ∼70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ∼28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.",
author = "Cauley, {P. Wilson} and Seth Redfield and Jensen, {Adam G.} and Travis Barman and Michael Endl and Cochran, {William D.}",
year = "2015",
month = "8",
day = "1",
doi = "10.1017/S1743921315010728",
language = "English (US)",
volume = "11",
pages = "376--381",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",
number = "S320",

}

TY - JOUR

T1 - Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b

AU - Cauley, P. Wilson

AU - Redfield, Seth

AU - Jensen, Adam G.

AU - Barman, Travis

AU - Endl, Michael

AU - Cochran, William D.

PY - 2015/8/1

Y1 - 2015/8/1

N2 - Hot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ∼70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ∼28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.

AB - Hot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ∼70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ∼28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.

UR - http://www.scopus.com/inward/record.url?scp=85054252712&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85054252712&partnerID=8YFLogxK

U2 - 10.1017/S1743921315010728

DO - 10.1017/S1743921315010728

M3 - Article

AN - SCOPUS:85054252712

VL - 11

SP - 376

EP - 381

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S320

ER -