Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

被引：14

作者：

Oliveira, J. Marques ^{[1
]}

Sicardy, B. ^{[1
]}

Gomes-Junior, A. R. ^{[2
,3
]}

Ortiz, J. L. ^{[4
]}

Strobel, D. F. ^{[5
,6
]}

Bertrand, T. ^{[1
,7
]}

Forget, F. ^{[8
]}

Lellouch, E. ^{[1
]}

Desmars, J. ^{[9
,10
]}

Berard, D. ^{[1
]}

Doressoundiram, A. ^{[1
]}

Lecacheux, J. ^{[1
]}

Leiva, R. ^{[11
,12
]}

Meza, E. ^{[13
,14
]}

Roques, F. ^{[1
]}

Souami, D. ^{[1
,15
]}

Widemann, T. ^{[1
]}

Santos-Sanz, P. ^{[4
]}

Morales, N. ^{[4
]}

Duffard, R. ^{[4
]}

Fernandez-Valenzuela, E. ^{[4
,16
]}

Castro-Tirado, A. J. ^{[4
]}

Braga-Ribas, F. ^{[1
,3
,17
,18
]}

Morgado, B. E. ^{[1
,3
,18
]}

Assafin, M. ^{[3
,19
]}

Camargo, J. I. B. ^{[3
,18
]}

Vieira-Martins, R. ^{[3
,10
,18
]}

Benedetti-Rossi, G. ^{[1
,2
,3
]}

Santos-Filho, S. ^{[3
,19
]}

Banda-Huarca, M., V ^{[3
,18
]}

Quispe-Huaynasi, F. ^{[18
]}

Pereira, C. L. ^{[3
,18
]}

Rommel, F. L. ^{[3
,18
]}

Margoti, G. ^{[17
]}

Dias-Oliveira, A. ^{[20
]}

Colas, F. ^{[10
]}

Berthier, J. ^{[10
]}

Renner, S. ^{[10
,21
]}

Hueso, R. ^{[22
]}

Perez-Hoyos, S. ^{[22
]}

Sanchez-Lavega, A. ^{[22
]}

Rojas, J. F. ^{[22
]}

Beisker, W. ^{[23
,24
]}

Kretlow, M. ^{[4
,23
,24
]}

Herald, D. ^{[25
,26
]}

Gault, D. ^{[25
]}

Bath, K-L ^{[23
,24
]}

Bode, H-J ^{[23
,24
]}

Bredner, E. ^{[24
,27
,28
,29
]}

Guhl, K. ^{[24
,30
]}

机构：

[1] Sorbonne Univ, Univ PSL, Observ Paris, CNRS,LESIA, 5 Pl Jules Janssen, F-92190 Meudon, France

[2] UNESP Sao Paulo State Univ, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil

[3] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[4] Inst Astrofis Andalucia IAA CSIC, Glorieta Astron S-N, Granada 18008, Spain

[5] Johns Hopkins Univ, Dept Earth & Planetary Sci, 3400 N Charles St, Baltimore, MD 21218 USA

[6] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA

[7] NASA, Ames Res Ctr, Space Sci Div, Moffett Field, CA 94035 USA

[8] Univ PSL, Sorbonne Univ, Lab Meteorol Dynam, CNRS,IPSL, 4 Pl Jussieu, F-5005 Paris, France

[9] Inst Polytech Sci Avancees IPSA, 63 Blvd Brandebourg, F-94200 Ivry, France

[10] Univ PSL, Sorbonne Univ, IMCCE Observ Paris, CNRS,Univ Lille, 77 Ave Denfert Rochereau, F-5014 Paris, France

[11] Univ Cote Azur, Observ Cote Azur, Lab Lagrange, CNRS, Bd Observ,CS 34229, F-06304 Nice 4, France

[12] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile

[13] Comis Nacl Invest & Desarrollo Aerosp Peru CONIDA, Lima, Peru

[14] Observ Astron Moquegua, Moquegua, Peru

[15] Univ Namur, naXys, 8 Rempart de la Vierge, B-5000 Namur, Belgium

[16] Univ Cent Florida, Florida Space Inst, 12354 Res Pkwy,Partnership 1, Orlando, FL 32816 USA

[17] Fed Univ Technol Parana UTFPR DAFIS, Curitiba, Parana, Brazil

[18] Observ Nacl MCTIC, Rio De Janeiro, Brazil

[19] Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ, Brazil

[20] Polo Educ Sesc, Av Ayrton Senna 5677, BR-225004 Rio De Janeiro, Brazil

[21] Univ Lille, Observ Lille, 1 Impasse Observ, F-59000 Lille, France

[22] Univ Pais Vasco UPV EHU, Dept Fis Aplicada, Escuela Ingn Bilbao, Plaza Ingeniero Torres Quevedo 1, Bilbao 48013, Spain

[23] Int Amateursternwarte IAS eV, Mittelstr 6, D-15749 Mittenwalde, Germany

[24] Int Occultat Timing Assoc European Sect IOTA ES, Brombeerhag 13, D-30459 Hannover, Germany

[25] Transtasman Occultat Alliance TTOA, POB 2241, Wellington, New Zealand

[26] Int Occultat Timing Assoc, POB 152, Kent, WA 98042 USA

[27] Vereinigung Sternfreunde eV VdS, Heppenheim, Germany

[28] St Sulpice Observ, Club Eclipse, 102 Rue Vaugirard, F-75006 Paris, France

[29] Dutch Occultat Assoc, Dutch Observers Asteroids DOA, Roden, Netherlands

[30] Archenhold Sternwarte, Alt Treptow 1, D-12435 Berlin, Germany

[31] British Astron Assoc, Burlington House, London W1J 0DU, England

[32] European Space Agcy ESA, ESTEC SCI S, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[33] Natl & Kapodistrian Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, Athens 15784, Greece

[34] Hellen Amateur Astron Assoc, Athens, Greece

[35] Armagh Observ & Planetarium, Armagh, North Ireland

[36] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Athens 15236, Greece

[37] Univ Crete, Dept Phys, Iraklion 71003, Greece

[38] Fdn Res & Technol Hellas, Inst Astrophys, Iraklion 70013, Greece

[39] Czech Acad Sci, Astron Inst, Fricova 298, Ondrejov 25165, Czech Republic

[40] Sternwarte Stuttgart, Stuttgart, Germany

[41] Hieronymusstr 15b, D-81241 Munich, Germany

[42] Astron Arbeitsgemeinschaft Wanne Eickel Herne eV, Breitenweg, Germany

[43] Rosenfeld Brittheim eV, Observ Sternwarte Zollern Alb, Rosenfeld, Germany

[44] AVV Astron Vereinigung Vulkaneifel Astron Soc Vol, Schalkenmehren, Germany

[45] Ariel Univ, Dept Phys, IL-40700 Ariel, Israel

[46] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[47] Selztal Observ, Friesenheim, Bechtolsheimer, Germany

[48] Bochumer Herbsttagung Amateuratsronomen BoHeTa, Bochum, Germany

[49] Gesell Volkstumliche Astron eV Hamburg, Hammerichstr 5, D-22605 Hamburg, Germany

[50] EURASTER, Grp Astrofili Massesi, Massa, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 659卷

基金：

欧洲研究理事会; 巴西圣保罗研究基金会; 欧盟地平线“2020”; 英国科学技术设施理事会;

关键词：

methods: data analysis; methods: observational; planets and satellites: atmospheres; planets and satellites: physical evolution; techniques: photometric; PLUTOS ATMOSPHERE; THERMAL STRUCTURE; DENSITY PROFILES; NITROGEN ICE; TEMPERATURE; HAZE; SURFACE; PHOTOCHEMISTRY; SATELLITES; PRESSURE;

D O I：

10.1051/0004-6361/202141443

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude.

引用

页数：43

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