Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA

M. A. Cordiner; S. B. Charnley; M. J. Mumma; D. Bockelée-Morvan; N. Biver; G. Villanueva; L. Paganini; S. N. Milam; A. J. Remijan; D. C. Lis; J. Crovisier; J. Boissier; Y. J. Kuan; I. M. Coulson

doi:10.1017/S1743921316002957

Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA

M. A. Cordiner, S. B. Charnley, M. J. Mumma, D. Bockelée-Morvan, N. Biver, G. Villanueva, L. Paganini, S. N. Milam, A. J. Remijan, D. C. Lis, J. Crovisier, J. Boissier, Y. J. Kuan, I. M. Coulson

地球科學系(含海洋環境研究所)

研究成果: 雜誌貢獻 › 期刊論文 › 同行評審

2 引文斯高帕斯（Scopus）

摘要

The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH3OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH3OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH3OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH3OH rotational temperature (T rot) as a function of sky-projected nucleocentric distance (ρ), fell by about 40 K between ρ= 0 and 2500 km on 28 June, whereas on 29 June, T rot fell by about 50 K between ρ =0 km and 1500 km. A remarkable (~50 K) rise in T rot at ρ = 1500-2500 km on 29 June was not present on 28 June. The observed variations in CH3OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role.

原文	英語
頁（從 - 到）	233-236
頁數	4
期刊	Proceedings of the International Astronomical Union
卷	11
發行號	A29A
DOIs	https://doi.org/10.1017/S1743921316002957
出版狀態	已發佈 - 2015

ASJC Scopus subject areas

天文和天體物理學
空間與行星科學

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Cordiner, M. A., Charnley, S. B., Mumma, M. J., Bockelée-Morvan, D., Biver, N., Villanueva, G., Paganini, L., Milam, S. N., Remijan, A. J., Lis, D. C., Crovisier, J., Boissier, J., Kuan, Y. J., & Coulson, I. M. (2015). Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA. Proceedings of the International Astronomical Union, 11(A29A), 233-236. https://doi.org/10.1017/S1743921316002957

Cordiner, MA, Charnley, SB, Mumma, MJ, Bockelée-Morvan, D, Biver, N, Villanueva, G, Paganini, L, Milam, SN, Remijan, AJ, Lis, DC, Crovisier, J, Boissier, J, Kuan, YJ & Coulson, IM 2015, 'Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA', Proceedings of the International Astronomical Union, 卷 11, 編號 A29A, 頁 233-236. https://doi.org/10.1017/S1743921316002957

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abstract = "The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH3OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH3OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH3OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH3OH rotational temperature (T rot) as a function of sky-projected nucleocentric distance (ρ), fell by about 40 K between ρ= 0 and 2500 km on 28 June, whereas on 29 June, T rot fell by about 50 K between ρ =0 km and 1500 km. A remarkable (~50 K) rise in T rot at ρ = 1500-2500 km on 29 June was not present on 28 June. The observed variations in CH3OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role.",

keywords = "Comets: individual (C/2012 K1 (PanSTARRS), molecular processes, submillimeter, techniques: interferometric",

author = "Cordiner, {M. A.} and Charnley, {S. B.} and Mumma, {M. J.} and D. Bockel{\'e}e-Morvan and N. Biver and G. Villanueva and L. Paganini and Milam, {S. N.} and Remijan, {A. J.} and Lis, {D. C.} and J. Crovisier and J. Boissier and Kuan, {Y. J.} and Coulson, {I. M.}",

note = "Publisher Copyright: Copyright {\textcopyright} International Astronomical Union 2016.",

year = "2015",

doi = "10.1017/S1743921316002957",

language = "English",

volume = "11",

pages = "233--236",

journal = "Proceedings of the International Astronomical Union",

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number = "A29A",

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T1 - Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA

AU - Cordiner, M. A.

AU - Charnley, S. B.

AU - Mumma, M. J.

AU - Bockelée-Morvan, D.

AU - Biver, N.

AU - Villanueva, G.

AU - Paganini, L.

AU - Milam, S. N.

AU - Remijan, A. J.

AU - Lis, D. C.

AU - Crovisier, J.

AU - Boissier, J.

AU - Kuan, Y. J.

AU - Coulson, I. M.

PY - 2015

Y1 - 2015

N2 - The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH3OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH3OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH3OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH3OH rotational temperature (T rot) as a function of sky-projected nucleocentric distance (ρ), fell by about 40 K between ρ= 0 and 2500 km on 28 June, whereas on 29 June, T rot fell by about 50 K between ρ =0 km and 1500 km. A remarkable (~50 K) rise in T rot at ρ = 1500-2500 km on 29 June was not present on 28 June. The observed variations in CH3OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role.

AB - The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH3OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH3OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH3OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH3OH rotational temperature (T rot) as a function of sky-projected nucleocentric distance (ρ), fell by about 40 K between ρ= 0 and 2500 km on 28 June, whereas on 29 June, T rot fell by about 50 K between ρ =0 km and 1500 km. A remarkable (~50 K) rise in T rot at ρ = 1500-2500 km on 29 June was not present on 28 June. The observed variations in CH3OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role.

KW - Comets: individual (C/2012 K1 (PanSTARRS)

KW - molecular processes

KW - submillimeter

KW - techniques: interferometric

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JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

IS - A29A

ER -

Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA

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