Structure and evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko | Zendy

Charlotte Goetz | Zendy; C. Koenders | Zendy; K. C. Hansen | Zendy; J. L. Burch | Zendy; C. Carr | Zendy; A. I. Eriksson | Zendy; Dennis Frühauff | Zendy; C. Güttler | Zendy; Pierre Henri | Zendy; H. Nilsson | Zendy; Ingo Richter | Zendy; M. Rubı́n | Zendy; H. Sierks | Zendy; B. T. Tsurutani | Zendy; M. Volwerk | Zendy; KarlHeinz Glaßmeier | Zendy

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Structure and evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko

Author(s) -

Charlotte Goetz,

C. Koenders,

K. C. Hansen,

J. L. Burch,

C. Carr,

A. I. Eriksson,

Dennis Frühauff,

C. Güttler,

Pierre Henri,

H. Nilsson,

Ingo Richter,

M. Rubı́n,

H. Sierks,

B. T. Tsurutani,

M. Volwerk,

KarlHeinz Glaßmeier

Publication year - 2016

Publication title -

monthly notices of the royal astronomical society

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.058

H-Index - 383

eISSN - 1365-8711

pISSN - 0035-8711

DOI - 10.1093/mnras/stw3148

Subject(s) - physics , outgassing , comet , diamagnetism , astrophysics , boundary (topology) , cavity wall , instability , computational physics , magnetic field , astronomy , mechanics , quantum mechanics , mathematical analysis , materials science , mathematics , composite material

The long duration of the Rosetta mission allows us to study the evolution of the diamagnetic cavity at comet 67P/Churyumov-Gerasimenko in detail. From 2015 April to 2016 February 665 intervals could be identified where Rosetta was located in a zero-magnetic-field region. We study the temporal and spatial distribution of this cavity and its boundary and conclude that the cavity properties depend on the long-term trend of the outgassing rate, but do not respond to transient events at the spacecraft location, such as outbursts or high neutral densities. Using an empirical model of the outgassing rate, we find a functional relationship between the outgassing rate and the distance of the cavity to the nucleus. There is also no indication that this unexpectedly large distance is related to unusual solar wind conditions. Because the deduced shape of the cavity boundary is roughly elliptical on small scales and the distances of the boundary from the nucleus are much larger than expected we conclude that the events observed by Rosetta are due to a moving instability of the cavity boundary itself

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