C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST03:38:21

2014A&A...568A..61S - Astronomy and Astrophysics, volume 568A, 61-61 (2014/8-1)

Multifrequency analysis of the Jovian electron-belt radiation during the Cassini flyby of Jupiter.


Abstract (from CDS):

We examine Very Large Array (VLA) observations of Jupiter to present evidence of fluctuations in the emission produced by the electron belt in January 2001. Investigating the source of fluctuations will provide new opportunities to discuss the scenarios of temporal changes in Jupiter's synchrotron radiation (i.e., the electron belt) in future data analysis and modeling work. To discuss the electron belt dynamics during the Cassini flyby of Jupiter, we compare the radio measurements from 2-3 January 2001 with VLA observations obtained on 20-21 December 1988, when viewing geometry and array configuration are comparable. All data are scaled to a standard Earth-Jupiter distance of 4.04AU for comparison purposes. Brightness distribution maps with identical spatial resolutions and cartography of the equatorial radiation are constructed and examined at the wavelengths of ∼21cm and ∼90cm. Rotation-averaged maps show that the emission from the equatorial zones of maximum intensity is weaker by ∼5-40%, but the brightness distribution is spatially more extended on 2-3 January 2001, resulting in a total emission at both wavelengths stronger by ∼35%. Between observation periods, the brightness distributions are observed to evolve differently during the planet rotation. Tomographic reconstructions of the equatorial radiation support our conclusion that the electron-belt population was differently distributed around the planet in December 1988 and January 2001. Our analysis of VLA data sets suggests that the spatial distribution of the electron belt on 2-3 January 2001 is different from that usually observed. Our knowledge of solar activity at the time of the Cassini flyby of Jupiter suggests that the emission from the electron radiation belt was responding to external influences, most likely to solar wind structures rather than to solar radio flux, on a timescale of days to a couple of weeks. Combined results from a multisource data analysis - including spacecraft and radio observations - are needed to confirm this relationship.

Abstract Copyright:

Journal keyword(s): radiation mechanisms: non-thermal - methods: data analysis

Simbad objects: 3

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Number of rows : 3

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
1 3C 48 QSO 01 37 41.2995845985 +33 09 35.079126038   16.62 16.20     ~ 2429 2
2 ICRF J031857.8+162832 AGN 03 18 57.80262301 +16 28 32.6981890     22.0     ~ 186 1
3 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3614 1

    Equat.    Gal    SGal    Ecl

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