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The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets

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The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets. / Arridge, C. S.; Achilleos, N.; Agarwal, J. et al.
In: Planetary and Space Science, Vol. 104, No. Part A, 12.2014, p. 122-140.

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

Harvard

Arridge, CS, Achilleos, N, Agarwal, J, Agnor, CB, Ambrosi, R, Andre, N, Badman, SV, Baines, K, Banfield, D, Barthelemy, M, Bisi, MM, Blum, J, Bocanegra-Bahamon, T, Bonfond, B, Bracken, C, Brandt, P, Briand, C, Briois, C, Brooks, S, Castillo-Rogez, J, Cavalie, T, Christophe, B, Coates, AJ, Collinson, G, Cooper, JF, Costa-Sitja, M, Courtin, R, Daglis, IA, De Pater, I, Desai, M, Dirkx, D, Dougherty, MK, Ebert, RW, Filacchione, G, Fletcher, LN, Fortney, J, Gerth, I, Grassi, D, Grodent, D, Grun, E, Gustin, J, Hedman, M, Helled, R, Henri, P, Hess, S, Hillier, JK, Hofstadter, MH, Holme, R, Horanyi, M, Hospodarsky, G, Hsu, S, Irwin, P, Jackman, CM, Karatekin, O, Kempf, S, Khalisi, E, Konstantinidis, K, Kruger, H, Kurth, WS, Labrianidis, C, Lainey, V, Lamy, LL, Laneuville, M, Lucchesi, D, Luntzer, A, MacArthur, J, Maier, A, Masters, A, McKenna-Lawlor, S, Melin, H, Milillo, A, Moragas-Klostermeyer, G, Morschhauser, A, Moses, JI, Mousis, O, Nettelmann, N, Neubauer, FM, Nordheim, T, Noyelles, B, Orton, GS, Owens, M, Peron, R, Plainaki, C, Postberg, F, Rambaux, N, Retherford, K, Reynaud, S, Roussos, E, Russell, CT, Rymer, A, Sallantin, R, Sanchez-Lavega, A, Santolik, O, Saur, J, Sayanagi, K, Schenk, P, Schubert, J, Sergis, N, Sittler, EC, Smith, A, Spahn, F, Srama, R, Stallard, T, Sterken, V, Sternovsky, Z, Tiscareno, M, Tobie, G, Tosi, F, Trieloff, M, Turrini, D, Turtle, EP, Vinatier, S, Wilson, R & Zarkat, P 2014, 'The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets', Planetary and Space Science, vol. 104, no. Part A, pp. 122-140. https://doi.org/10.1016/j.pss.2014.08.009

APA

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., ... Zarkat, P. (2014). The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets. Planetary and Space Science, 104(Part A), 122-140. https://doi.org/10.1016/j.pss.2014.08.009

Vancouver

Arridge CS, Achilleos N, Agarwal J, Agnor CB, Ambrosi R, Andre N et al. The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets. Planetary and Space Science. 2014 Dec;104(Part A):122-140. Epub 2014 Aug 22. doi: 10.1016/j.pss.2014.08.009

Author

Arridge, C. S. ; Achilleos, N. ; Agarwal, J. et al. / The science case for an orbital mission to Uranus : exploring the origins and evolution of ice giant planets. In: Planetary and Space Science. 2014 ; Vol. 104, No. Part A. pp. 122-140.

Bibtex

@article{2379945ab4fc497dbb0eecca88668fea,
title = "The science case for an orbital mission to Uranus: exploring the origins and evolution of ice giant planets",
abstract = "Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.",
keywords = "Uranus, Magnetosphere, Atmosphere, Natural satellites, Rings, Planetary interior, IRREGULAR SATELLITES SYCORAX, INNER URANIAN SATELLITES, MAGNETIC-FIELDS, SOLAR-SYSTEM, SUBSURFACE OCEANS, OUTER PLANETS, WATER ICE, E-RING, NEPTUNE, DYNAMICS",
author = "Arridge, {C. S.} and N. Achilleos and J. Agarwal and Agnor, {C. B.} and R. Ambrosi and N. Andre and Badman, {S. V.} and K. Baines and D. Banfield and M. Barthelemy and Bisi, {M. M.} and J. Blum and T. Bocanegra-Bahamon and Bonfond, {B. .} and C. Bracken and P. Brandt and C. Briand and C. Briois and S. Brooks and J. Castillo-Rogez and T. Cavalie and B. Christophe and Coates, {A. J.} and G. Collinson and Cooper, {J. F.} and M. Costa-Sitja and R. Courtin and Daglis, {I. A.} and {De Pater}, I. and M. Desai and D. Dirkx and Dougherty, {M. K.} and Ebert, {R. W.} and G. Filacchione and Fletcher, {L. N.} and J. Fortney and I. Gerth and D. Grassi and D. Grodent and E. Grun and J. Gustin and M. Hedman and R. Helled and P. Henri and S. Hess and Hillier, {J. K.} and Hofstadter, {M. H.} and R. Holme and M. Horanyi and G. Hospodarsky and S. Hsu and P. Irwin and Jackman, {C. M.} and O. Karatekin and S. Kempf and E. Khalisi and K. Konstantinidis and H. Kruger and Kurth, {W. S.} and C. Labrianidis and V. Lainey and Lamy, {L. L.} and M. Laneuville and D. Lucchesi and A. Luntzer and J. MacArthur and A. Maier and A. Masters and S. McKenna-Lawlor and H. Melin and A. Milillo and G. Moragas-Klostermeyer and A. Morschhauser and Moses, {J. I.} and O. Mousis and N. Nettelmann and Neubauer, {F. M.} and T. Nordheim and B. Noyelles and Orton, {G. S.} and M. Owens and R. Peron and C. Plainaki and F. Postberg and N. Rambaux and K. Retherford and S. Reynaud and E. Roussos and Russell, {C. T.} and Am. Rymer and R. Sallantin and A. Sanchez-Lavega and O. Santolik and J. Saur and Km. Sayanagi and P. Schenk and J. Schubert and N. Sergis and Sittler, {E. C.} and A. Smith and F. Spahn and R. Srama and T. Stallard and V. Sterken and Z. Sternovsky and M. Tiscareno and G. Tobie and F. Tosi and M. Trieloff and D. Turrini and Turtle, {E. P.} and S. Vinatier and R. Wilson and P. Zarkat",
year = "2014",
month = dec,
doi = "10.1016/j.pss.2014.08.009",
language = "English",
volume = "104",
pages = "122--140",
journal = "Planetary and Space Science",
issn = "0032-0633",
publisher = "Elsevier Limited",
number = "Part A",

}

RIS

TY - JOUR

T1 - The science case for an orbital mission to Uranus

T2 - exploring the origins and evolution of ice giant planets

AU - Arridge, C. S.

AU - Achilleos, N.

AU - Agarwal, J.

AU - Agnor, C. B.

AU - Ambrosi, R.

AU - Andre, N.

AU - Badman, S. V.

AU - Baines, K.

AU - Banfield, D.

AU - Barthelemy, M.

AU - Bisi, M. M.

AU - Blum, J.

AU - Bocanegra-Bahamon, T.

AU - Bonfond, B. .

AU - Bracken, C.

AU - Brandt, P.

AU - Briand, C.

AU - Briois, C.

AU - Brooks, S.

AU - Castillo-Rogez, J.

AU - Cavalie, T.

AU - Christophe, B.

AU - Coates, A. J.

AU - Collinson, G.

AU - Cooper, J. F.

AU - Costa-Sitja, M.

AU - Courtin, R.

AU - Daglis, I. A.

AU - De Pater, I.

AU - Desai, M.

AU - Dirkx, D.

AU - Dougherty, M. K.

AU - Ebert, R. W.

AU - Filacchione, G.

AU - Fletcher, L. N.

AU - Fortney, J.

AU - Gerth, I.

AU - Grassi, D.

AU - Grodent, D.

AU - Grun, E.

AU - Gustin, J.

AU - Hedman, M.

AU - Helled, R.

AU - Henri, P.

AU - Hess, S.

AU - Hillier, J. K.

AU - Hofstadter, M. H.

AU - Holme, R.

AU - Horanyi, M.

AU - Hospodarsky, G.

AU - Hsu, S.

AU - Irwin, P.

AU - Jackman, C. M.

AU - Karatekin, O.

AU - Kempf, S.

AU - Khalisi, E.

AU - Konstantinidis, K.

AU - Kruger, H.

AU - Kurth, W. S.

AU - Labrianidis, C.

AU - Lainey, V.

AU - Lamy, L. L.

AU - Laneuville, M.

AU - Lucchesi, D.

AU - Luntzer, A.

AU - MacArthur, J.

AU - Maier, A.

AU - Masters, A.

AU - McKenna-Lawlor, S.

AU - Melin, H.

AU - Milillo, A.

AU - Moragas-Klostermeyer, G.

AU - Morschhauser, A.

AU - Moses, J. I.

AU - Mousis, O.

AU - Nettelmann, N.

AU - Neubauer, F. M.

AU - Nordheim, T.

AU - Noyelles, B.

AU - Orton, G. S.

AU - Owens, M.

AU - Peron, R.

AU - Plainaki, C.

AU - Postberg, F.

AU - Rambaux, N.

AU - Retherford, K.

AU - Reynaud, S.

AU - Roussos, E.

AU - Russell, C. T.

AU - Rymer, Am.

AU - Sallantin, R.

AU - Sanchez-Lavega, A.

AU - Santolik, O.

AU - Saur, J.

AU - Sayanagi, Km.

AU - Schenk, P.

AU - Schubert, J.

AU - Sergis, N.

AU - Sittler, E. C.

AU - Smith, A.

AU - Spahn, F.

AU - Srama, R.

AU - Stallard, T.

AU - Sterken, V.

AU - Sternovsky, Z.

AU - Tiscareno, M.

AU - Tobie, G.

AU - Tosi, F.

AU - Trieloff, M.

AU - Turrini, D.

AU - Turtle, E. P.

AU - Vinatier, S.

AU - Wilson, R.

AU - Zarkat, P.

PY - 2014/12

Y1 - 2014/12

N2 - Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

AB - Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

KW - Uranus

KW - Magnetosphere

KW - Atmosphere

KW - Natural satellites

KW - Rings

KW - Planetary interior

KW - IRREGULAR SATELLITES SYCORAX

KW - INNER URANIAN SATELLITES

KW - MAGNETIC-FIELDS

KW - SOLAR-SYSTEM

KW - SUBSURFACE OCEANS

KW - OUTER PLANETS

KW - WATER ICE

KW - E-RING

KW - NEPTUNE

KW - DYNAMICS

U2 - 10.1016/j.pss.2014.08.009

DO - 10.1016/j.pss.2014.08.009

M3 - Journal article

VL - 104

SP - 122

EP - 140

JO - Planetary and Space Science

JF - Planetary and Space Science

SN - 0032-0633

IS - Part A

ER -