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Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+

Research output: Contribution to Journal/Magazine › Journal article › peer-review

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Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+. / Stallard, T. S.; Melin, H.; Miller, S. et al.
In: Philosophical Transactions A: Mathematical, Physical and Engineering Sciences , Vol. 370, No. 1978, 13.11.2012, p. 5213-5224.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Stallard, TS, Melin, H, Miller, S, O' Donoghue, J, Cowley, SWH, Badman, SV, Adriani, A, Brown, RH & Baines, KH 2012, 'Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+', Philosophical Transactions A: Mathematical, Physical and Engineering Sciences , vol. 370, no. 1978, pp. 5213-5224. https://doi.org/10.1098/rsta.2012.0028

APA

Stallard, T. S., Melin, H., Miller, S., O' Donoghue, J., Cowley, S. W. H., Badman, S. V., Adriani, A., Brown, R. H., & Baines, K. H. (2012). Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+. Philosophical Transactions A: Mathematical, Physical and Engineering Sciences , 370(1978), 5213-5224. https://doi.org/10.1098/rsta.2012.0028

Vancouver

Stallard TS, Melin H, Miller S, O' Donoghue J, Cowley SWH, Badman SV et al. Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+. Philosophical Transactions A: Mathematical, Physical and Engineering Sciences . 2012 Nov 13;370(1978):5213-5224. doi: 10.1098/rsta.2012.0028

Author

Stallard, T. S. ; Melin, H. ; Miller, S. et al. / Temperature changes and energy inputs in giant planet atmospheres : what we are learning from H3+. In: Philosophical Transactions A: Mathematical, Physical and Engineering Sciences . 2012 ; Vol. 370, No. 1978. pp. 5213-5224.

Bibtex

@article{786538aea5034033876d238df4c6a431,
title = "Temperature changes and energy inputs in giant planet atmospheres: what we are learning from H3+",
abstract = "Since its discovery at Jupiter in 1988, emission from HGraphic has been used as a valuable diagnostic tool in our understanding of the upper atmospheres of the giant planets. One of the lasting questions we have about the giant planets is why the measured upper atmosphere temperatures are always consistently hotter than the temperatures expected from solar heating alone. Here, we describe how HGraphic forms across each of the planetary disks of Jupiter, Saturn and Uranus, presenting the first observations of equatorial HGraphic at Saturn and the first profile of HGraphic emission at Uranus not significantly distorted by the effects of the Earth's atmosphere. We also review past observations of variations in temperature measured at Uranus and Jupiter over a wide variety of time scales. To this, we add new observations of temperature changes at Saturn, using observations by Cassini. We conclude that the causes of the significant level of thermal variability observed over all three planets is not only an important question in itself, but that explaining these variations could be the key to answering the more general question of why giant planet upper atmospheres are so hot.",
keywords = "aurora, aeronomy, Jupiter, Saturn, Uranus",
author = "Stallard, {T. S.} and H. Melin and S. Miller and {O' Donoghue}, J. and Cowley, {S. W. H.} and Badman, {S. V.} and A. Adriani and Brown, {R. H.} and Baines, {K. H.}",
year = "2012",
month = nov,
day = "13",
doi = "10.1098/rsta.2012.0028",
language = "English",
volume = "370",
pages = "5213--5224",
journal = "Philosophical Transactions A: Mathematical, Physical and Engineering Sciences ",
issn = "1364-503X",
publisher = "Royal Society of London",
number = "1978",

}

RIS

TY - JOUR

T1 - Temperature changes and energy inputs in giant planet atmospheres

T2 - what we are learning from H3+

AU - Stallard, T. S.

AU - Melin, H.

AU - Miller, S.

AU - O' Donoghue, J.

AU - Cowley, S. W. H.

AU - Badman, S. V.

AU - Adriani, A.

AU - Brown, R. H.

AU - Baines, K. H.

PY - 2012/11/13

Y1 - 2012/11/13

N2 - Since its discovery at Jupiter in 1988, emission from HGraphic has been used as a valuable diagnostic tool in our understanding of the upper atmospheres of the giant planets. One of the lasting questions we have about the giant planets is why the measured upper atmosphere temperatures are always consistently hotter than the temperatures expected from solar heating alone. Here, we describe how HGraphic forms across each of the planetary disks of Jupiter, Saturn and Uranus, presenting the first observations of equatorial HGraphic at Saturn and the first profile of HGraphic emission at Uranus not significantly distorted by the effects of the Earth's atmosphere. We also review past observations of variations in temperature measured at Uranus and Jupiter over a wide variety of time scales. To this, we add new observations of temperature changes at Saturn, using observations by Cassini. We conclude that the causes of the significant level of thermal variability observed over all three planets is not only an important question in itself, but that explaining these variations could be the key to answering the more general question of why giant planet upper atmospheres are so hot.

AB - Since its discovery at Jupiter in 1988, emission from HGraphic has been used as a valuable diagnostic tool in our understanding of the upper atmospheres of the giant planets. One of the lasting questions we have about the giant planets is why the measured upper atmosphere temperatures are always consistently hotter than the temperatures expected from solar heating alone. Here, we describe how HGraphic forms across each of the planetary disks of Jupiter, Saturn and Uranus, presenting the first observations of equatorial HGraphic at Saturn and the first profile of HGraphic emission at Uranus not significantly distorted by the effects of the Earth's atmosphere. We also review past observations of variations in temperature measured at Uranus and Jupiter over a wide variety of time scales. To this, we add new observations of temperature changes at Saturn, using observations by Cassini. We conclude that the causes of the significant level of thermal variability observed over all three planets is not only an important question in itself, but that explaining these variations could be the key to answering the more general question of why giant planet upper atmospheres are so hot.

KW - aurora

KW - aeronomy

KW - Jupiter

KW - Saturn

KW - Uranus

U2 - 10.1098/rsta.2012.0028

DO - 10.1098/rsta.2012.0028

M3 - Journal article

VL - 370

SP - 5213

EP - 5224

JO - Philosophical Transactions A: Mathematical, Physical and Engineering Sciences

JF - Philosophical Transactions A: Mathematical, Physical and Engineering Sciences

SN - 1364-503X

IS - 1978

ER -