sid.inpe.br/mtc-m21c/2018/09.24.18.04-TDI A STUDY OF PLASMA WAVES IN THE INDUCED MAGNETOSPHERES OF MARS AND VENUS Adriane Marques de Souza Franco Doctorate Thesis of the Graduate Course in Space Geophysics, guided by Drs. Ezequiel Echer, Maurício José Alves Bolzam, and Wolfram Johannes Markus Fränz, approved in October 25, 2018. URL of the original document: <http://urlib.net/8JMKD3MGP3W34R/3RSM69S> INPE São José dos Campos 2018 PUBLISHED BY: Instituto Nacional de Pesquisas Espaciais - INPE Gabinete do Diretor (GBDIR) Serviço de Informação e Documentação (SESID) CEP 12.227-010 São José dos Campos - SP - Brasil Tel.:(012) 3208-6923/7348 E-mail: [email protected] BOARD OF PUBLISHING AND PRESERVATION OF INPE INTELLECTUAL PRODUCTION - CEPPII (PORTARIA No 176/2018/SEI-INPE): Chairperson: Dr. Marley Cavalcante de Lima Moscati - Centro de Previsão de Tempo e Estudos Climáticos (CGCPT) Members: Dra. 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URL of the original document: <http://urlib.net/8JMKD3MGP3W34R/3RSM69S> INPE São José dos Campos 2018 Cataloging in Publication Data Franco, Adriane Marques de Souza. F848e A study of plasma waves in the induced magnetospheres of Mars and Venus / Adriane Marques de Souza Franco. – São José dos Campos : INPE, 2018. xxx + 264 p. ; (sid.inpe.br/mtc-m21c/2018/09.24.18.04-TDI) Thesis (Doctorate in Space Geophysics) – Instituto Nacional de Pesquisas Espaciais, São José dos Campos, 2018. Guiding : Drs. Ezequiel Echer, Maurício José Alves Bolzam, and Wolfram Johannes Markus Fränz. 1. Mars and Venus induced magnetospheres. 2. Plasma waves. 3. Correlation length. 4. Atmospheric loss. I.Title. CDU 52-854:523.42/.43 Esta obra foi licenciada sob uma Licença Creative Commons Atribuição-NãoComercial 3.0 Não Adaptada. This work is licensed under a Creative Commons Attribution-NonCommercial 3.0 Unported License. ii Aluno (a): Adriane Marques de Souza Franco Título: "UM ESTUDO DE ONDAS DE PLASMA NAS MAGNETOSFERAS INDUZIDAS DE MARTE E VÊNUS" Aprovado (a) pela Banca Examinadora em cumprimento ao requisito exigido para obtenção do Titulo de Doutor(a) em Geofisica Espacial/Ciências do Ambiente Solar-Terrestre Dra. Maria Virginia Alves fiA•Làt.4.4.,42.ji.ut,o Presidente / INPE / SJCampos - SP ( ) Participação por Vídeo - Conferência /0 Aprovado ( ) Reprovado Dr. Ezequiel Echer O ntbdor(a) / INPE / SJCampos - SP ( ) Partkipação por Video - Conferência Aprovado ( ) Reprovado - Dr. Maurício José Alves Bolzam Orientador(a) / UF / Jatai - GO ( ) Participação por Video - Conferência Aprovado ( ) Reprovado Dr. Renato Sergio Dallaqua Membro da Banca / IMPE / S o José dos Campos - SP ( ) Participação por Video - Conferência .g2 Aprovado ( ) Reprovado Este trabalho foi aprovado por: ( ) maioria simples (,)( unanimidade São José dos Campos, 25 de outubro de 2018 Aprovado (a) pela Banca Examinadora em cumprimento ao requisito exigido para obtenção do Titulo de Doutor(e) em Geofísica Espacial/Ciênclas do Ambiente Solar-Terrestre Dr. Fábio Becker Guedes Membro da Banca - E / São José dos Campos - SP ( ) Participação por Video - Conferência /(X). Aprovado ( ) Reprovado Dr. Manilo Soares Marques Convidado(a)/ UFRN / Natal - ( ) Participação por Video - Conferência NO Aprovado ( ) Reprovado Dr. Edio da Costa Júnior iv 14 Convidado(a) / IFMG / O Preto - MG ( ) Participação por Video - Conferência ()( Aprovado ( ) Reprovado Este trabalho foi aprovado por: ( ) maioria simples X) unanimidade São José dos Campos, 25 de outubro de 2018 “If I have seen further than others, it is by standing upon the shoulders of giants”. Isaac Newton v vi I dedicate this thesis to my mother and father, and also to my husband Francis Franco for their endless support. vii viii ACKNOWLEDGMENTS First of all, I would like to thank God for make me feel strong and believe in myself in the moments that I needed. I thank my supervisors Dr. Ezequiel Echer, Dr. Mauricio José Alves Bolzam and Dr. Markus Fraenz to the orientation that was given in the development of this thesis that allowed it been completion. For all explanations, helps with methodology and patience with my limitations. To the INPE professors for all transmitted knowledge. To my colleagues: Anna Karina, Jenny Marcela, Fabiola Magalhães and Williamary Portugal for their attention, contributions to the development of this work and also for adventures in conferences. I also would like to thank my family and friends that always supported me. To the CAPES (Coordination for the Improvement of Higher Level – OR Education Personnel), and FAPESP (São Paulo Research Foundation, grants Nº 2016/10794-2 and Nº 2017/00516-8), for the financial support of my PhD. To the Max Planck institute for Solar System Research for receiving me during my sandwich fellowship and provides me all support that I needed to develop my research. To the National Institute for Space Research (INPE), for the opportunity and support in my formation. ix x ABSTRACT Plasma waves are considered as an essential factor in the physics of planetary magnetospheres, since they may transfer energy and momentum from the solar wind to the inner magnetospheric cavity. In Mars and Venus, where the magnetosphere is formed by the interaction of the solar wind with the upper atmosphere/ionosphere of the planet (induced magnetospheres), the low energy ion escape is mainly related to the extreme ultra-violet radiation and solar wind pressure. But the solar wind pressure and interaction with the planetary bow shock increases the wave production in the magnetosheath. It is unclear to what degree magnetic shielding can prevent that ultra low frequency waves generated in the sheath penetrate into the ionosphere. Thus, these waves may provide enough energy to accelerate ionospheric ions, so that they reach escape speed, contributing to the atmospheric erosion of the planet. In this thesis, these plasma waves have been studied in the induced magnetospheres of Mars and Venus using three different techniques: correlation lengths for both planets, wavelet transform in the identification of the main frequency of these waves in the magnetosheath of Mars and transport ratios to identify dominant wave modes for Venus. It was found that the main frequencies in the magnetosheath of Mars are in the range between 5 and 20 mHz. These frequencies did not show any dependence with the solar cycle. Correlation lengths around Mars were computed for Mars express (MEX) data (electron density from 2004 to 2015) and for Mars Atmosphere and Volatile Evolution Mission (MAVEN) data (electron density and magnetic field from 2014 to 2016). Correlation length in electron density data was found to be varying between 13 and 17 seconds (temporal scale) and between 5.5푥103km and 6.8푥103 km (spatial scale) for the MEX analysis. For MAVEN it varies between 11 and 16 seconds (temporal scale) and 2푥103 − 4.5푥103 km in spatial scale. In the magnetic field data, correlation lengths are observed between 8-15 seconds (temporal scale) and between 1푥103 and 5푥103 km (spatial scale). In Venus similar correlation lengths have been seen using Venus express (VEX) data (2006-2014). It varies from 9 to 14 seconds (temporal) and from 2.8푋103 to 5푋103km (spatial scale) in the electron density data. For magnetic field, correlation length was found between 7.5-11 seconds (temporal) and 1.7푥103- 4푋103km (spatial). For both planets it was seen that the sizes of the plasma regions are smaller than the observed correlation lengths observed inside them, which indicates that waves at the magnetosheath/magnetic pile-up region (MPR) can be related to oscillations in the ionosphere. In a local region, wave trains may cause resonance effects at the planetary ionopause, which consequently contributes to the enhanced ion escape from the atmosphere. For Mars, 29 cases of potential wave penetration into the ionosphere were identified. The predominant wave mode around Venus was the Alfvenic mode, xi which can be observed everywhere, mostly inside of the magnetosheath and in the upstream solar wind. Keywords: Mars and Venus Induced Magnetospheres. Plasma Waves. Correlation Length. Atmospheric Loss. xii ESTUDO DE ONDAS DE PLASMA NAS MAGNETOSFERAS INDUZIDAS DE MARTE E VENUS RESUMO Ondas de plasma são consideradas como um fator essencial na física magnetosférica, já que as mesmas podem transferir