A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION

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A DISTANT MIRROR : SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION. / Gaulme, P.; Rowe, J. F.; Bedding, T. R.; Benomar, O.; Corsaro, E.; Davies, G. R.; Hale, S. J.; Howe, R.; Garcia, R. A.; Huber, D.; Jiménez, A.; Mathur, S.; Mosser, B.; Appourchaux, T.; Boumier, P.; Jackiewicz, J.; Leibacher, J.; Schmider, F. X.; Hammel, H. B.; Lissauer, J. J.; Marley, M. S.; Simon, A. A.; Chaplin, W. J.; Elsworth, Y.; Guzik, J. A.; Murphy, N.; Aguirre, V. Silva.

In: Astrophysical Journal Letters, Vol. 833, No. 1, L13, 10.12.2016.

Research output: Contribution to journalArticlepeer-review

Harvard

Gaulme, P, Rowe, JF, Bedding, TR, Benomar, O, Corsaro, E, Davies, GR, Hale, SJ, Howe, R, Garcia, RA, Huber, D, Jiménez, A, Mathur, S, Mosser, B, Appourchaux, T, Boumier, P, Jackiewicz, J, Leibacher, J, Schmider, FX, Hammel, HB, Lissauer, JJ, Marley, MS, Simon, AA, Chaplin, WJ, Elsworth, Y, Guzik, JA, Murphy, N & Aguirre, VS 2016, 'A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION', Astrophysical Journal Letters, vol. 833, no. 1, L13. https://doi.org/10.3847/2041-8213/833/1/L13

APA

Gaulme, P., Rowe, J. F., Bedding, T. R., Benomar, O., Corsaro, E., Davies, G. R., Hale, S. J., Howe, R., Garcia, R. A., Huber, D., Jiménez, A., Mathur, S., Mosser, B., Appourchaux, T., Boumier, P., Jackiewicz, J., Leibacher, J., Schmider, F. X., Hammel, H. B., ... Aguirre, V. S. (2016). A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION. Astrophysical Journal Letters, 833(1), [L13]. https://doi.org/10.3847/2041-8213/833/1/L13

Vancouver

Author

Gaulme, P. ; Rowe, J. F. ; Bedding, T. R. ; Benomar, O. ; Corsaro, E. ; Davies, G. R. ; Hale, S. J. ; Howe, R. ; Garcia, R. A. ; Huber, D. ; Jiménez, A. ; Mathur, S. ; Mosser, B. ; Appourchaux, T. ; Boumier, P. ; Jackiewicz, J. ; Leibacher, J. ; Schmider, F. X. ; Hammel, H. B. ; Lissauer, J. J. ; Marley, M. S. ; Simon, A. A. ; Chaplin, W. J. ; Elsworth, Y. ; Guzik, J. A. ; Murphy, N. ; Aguirre, V. Silva. / A DISTANT MIRROR : SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION. In: Astrophysical Journal Letters. 2016 ; Vol. 833, No. 1.

Bibtex

@article{82b2cc7c9e14488c9d3c48d783eba214,
title = "A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION",
abstract = "Starting in 2014 December, Kepler K 2 observed Neptune continuously for 49 days at a 1 minute cadence. The goals consisted of studying its atmospheric dynamics, detecting its global acoustic oscillations, and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude ν max and the mean frequency separation between mode overtones Δν, is surprising as the ν max measured from Neptune photometry is larger than the accepted value. Compared to the usual reference ν max,o = 3100 μHz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 ±5.8% and 4.3 ±1.9%, respectively. The higher ν max is caused by a combination of the value of ν max,o, being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 ±10 μHz), and the noise level of the K 2 time series, being 10 times larger than VIRGO's. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (S/N), we model 10 overtones for degrees ℓ = 0, 1, 2. We compare the K 2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1σ, except for the few peaks with the lowest S/N.",
keywords = "planets and satellites: individual (Neptune), stars: oscillations (including pulsations), Sun: helioseismology, techniques: photometric",
author = "P. Gaulme and Rowe, {J. F.} and Bedding, {T. R.} and O. Benomar and E. Corsaro and Davies, {G. R.} and Hale, {S. J.} and R. Howe and Garcia, {R. A.} and D. Huber and A. Jim{\'e}nez and S. Mathur and B. Mosser and T. Appourchaux and P. Boumier and J. Jackiewicz and J. Leibacher and Schmider, {F. X.} and Hammel, {H. B.} and Lissauer, {J. J.} and Marley, {M. S.} and Simon, {A. A.} and Chaplin, {W. J.} and Y. Elsworth and Guzik, {J. A.} and N. Murphy and Aguirre, {V. Silva}",
year = "2016",
month = dec,
day = "10",
doi = "10.3847/2041-8213/833/1/L13",
language = "English",
volume = "833",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "Institute of Physics Publishing Ltd",
number = "1",

}

RIS

TY - JOUR

T1 - A DISTANT MIRROR

T2 - SOLAR OSCILLATIONS OBSERVED on NEPTUNE by the KEPLER K 2 MISSION

AU - Gaulme, P.

AU - Rowe, J. F.

AU - Bedding, T. R.

AU - Benomar, O.

AU - Corsaro, E.

AU - Davies, G. R.

AU - Hale, S. J.

AU - Howe, R.

AU - Garcia, R. A.

AU - Huber, D.

AU - Jiménez, A.

AU - Mathur, S.

AU - Mosser, B.

AU - Appourchaux, T.

AU - Boumier, P.

AU - Jackiewicz, J.

AU - Leibacher, J.

AU - Schmider, F. X.

AU - Hammel, H. B.

AU - Lissauer, J. J.

AU - Marley, M. S.

AU - Simon, A. A.

AU - Chaplin, W. J.

AU - Elsworth, Y.

AU - Guzik, J. A.

AU - Murphy, N.

AU - Aguirre, V. Silva

PY - 2016/12/10

Y1 - 2016/12/10

N2 - Starting in 2014 December, Kepler K 2 observed Neptune continuously for 49 days at a 1 minute cadence. The goals consisted of studying its atmospheric dynamics, detecting its global acoustic oscillations, and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude ν max and the mean frequency separation between mode overtones Δν, is surprising as the ν max measured from Neptune photometry is larger than the accepted value. Compared to the usual reference ν max,o = 3100 μHz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 ±5.8% and 4.3 ±1.9%, respectively. The higher ν max is caused by a combination of the value of ν max,o, being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 ±10 μHz), and the noise level of the K 2 time series, being 10 times larger than VIRGO's. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (S/N), we model 10 overtones for degrees ℓ = 0, 1, 2. We compare the K 2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1σ, except for the few peaks with the lowest S/N.

AB - Starting in 2014 December, Kepler K 2 observed Neptune continuously for 49 days at a 1 minute cadence. The goals consisted of studying its atmospheric dynamics, detecting its global acoustic oscillations, and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude ν max and the mean frequency separation between mode overtones Δν, is surprising as the ν max measured from Neptune photometry is larger than the accepted value. Compared to the usual reference ν max,o = 3100 μHz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 ±5.8% and 4.3 ±1.9%, respectively. The higher ν max is caused by a combination of the value of ν max,o, being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 ±10 μHz), and the noise level of the K 2 time series, being 10 times larger than VIRGO's. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (S/N), we model 10 overtones for degrees ℓ = 0, 1, 2. We compare the K 2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1σ, except for the few peaks with the lowest S/N.

KW - planets and satellites: individual (Neptune)

KW - stars: oscillations (including pulsations)

KW - Sun: helioseismology

KW - techniques: photometric

UR - http://www.scopus.com/inward/record.url?scp=85007018177&partnerID=8YFLogxK

U2 - 10.3847/2041-8213/833/1/L13

DO - 10.3847/2041-8213/833/1/L13

M3 - Article

AN - SCOPUS:85007018177

VL - 833

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 1

M1 - L13

ER -