[1712.07301] Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars

<!DOCTYPE html> <html lang="en"> <head> <title>[1712.07301] Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars</title> <meta name="viewport" content="width=device-width, initial-scale=1"> <link rel="apple-touch-icon" sizes="180x180" href="/static/browse/0.3.4/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="/static/browse/0.3.4/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="/static/browse/0.3.4/images/icons/favicon-16x16.png"> <link rel="manifest" href="/static/browse/0.3.4/images/icons/site.webmanifest"> <link rel="mask-icon" href="/static/browse/0.3.4/images/icons/safari-pinned-tab.svg" color="#5bbad5"> <meta name="msapplication-TileColor" content="#da532c"> <meta name="theme-color" content="#ffffff"> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/arXiv.css?v=20241206" /> <link rel="stylesheet" type="text/css" media="print" href="/static/browse/0.3.4/css/arXiv-print.css?v=20200611" /> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/browse_search.css" /> <script language="javascript" src="/static/browse/0.3.4/js/accordion.js" /></script> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/slider.css?v=20250312" /> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script type="text/javascript" src="/static/browse/0.3.4/js/donate.js?v=121124"></script><link rel="canonical" href="https://arxiv.org/abs/1712.07301"/> <meta name="description" content="Abstract page for arXiv paper 1712.07301: Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars"><meta property="og:type" content="website" /> <meta property="og:site_name" content="arXiv.org" /> <meta property="og:title" content="Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars" /> <meta property="og:url" content="https://arxiv.org/abs/1712.07301v1" /> <meta property="og:image" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:secure_url" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:width" content="1200" /> <meta property="og:image:height" content="700" /> <meta property="og:image:alt" content="arXiv logo"/> <meta property="og:description" content="The propagation of 15 interplanetary coronal mass ejections (ICMEs) from Earth's orbit (1 AU) to Mars (~ 1.5 AU) has been studied with their propagation speed estimated from both measurements and simulations. The enhancement of magnetic fields related to ICMEs and their shock fronts cause the so-called Forbush decrease, which can be de- tected as a reduction of galactic cosmic rays measured on-ground. We have used galactic cosmic ray (GCR) data from in-situ measurements at Earth, from both STEREO A and B as well as GCR measurements by the Radiation Assessment Detector (RAD) instrument onboard Mars Science Laboratory (MSL) on the surface of Mars. A set of ICME events has been selected during the periods when Earth (or STEREO A or B) and Mars locations were nearly aligned on the same side of the Sun in the ecliptic plane (so-called opposition phase). Such lineups allow us to estimate the ICMEs' transit times between 1 and 1.5 AU by estimating the delay time of the corresponding Forbush decreases measured at each location. We investigate the evolution of their propagation speeds before and after passing Earth's orbit and find that the deceleration of ICMEs due to their interaction with the ambient solar wind may continue beyond 1 AU. We also find a substantial variance of the speed evolution among different events revealing the dynamic and diverse nature of eruptive solar events. Furthermore, the results are compared to simulation data obtained from two CME propagation models, namely the Drag-Based Model and ENLIL plus cone model."/> <meta name="twitter:site" content="@arxiv"/> <meta name="twitter:card" content="summary"/> <meta name="twitter:title" content="Using Forbush decreases to derive the transit time of ICMEs..."/> <meta name="twitter:description" content="The propagation of 15 interplanetary coronal mass ejections (ICMEs) from Earth's orbit (1 AU) to Mars (~ 1.5 AU) has been studied with their propagation speed estimated from both measurements and..."/> <meta name="twitter:image" content="https://static.arxiv.org/icons/twitter/arxiv-logo-twitter-square.png"/> <meta name="twitter:image:alt" content="arXiv logo"/> <link rel="stylesheet" media="screen" type="text/css" href="/static/browse/0.3.4/css/tooltip.css"/><link rel="stylesheet" media="screen" type="text/css" href="https://static.arxiv.org/js/bibex-dev/bibex.css?20200709"/> <script src="/static/browse/0.3.4/js/mathjaxToggle.min.js" type="text/javascript"></script> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/js-cookie@2/src/js.cookie.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/dompurify@2.3.5/dist/purify.min.js"></script> <script src="/static/browse/0.3.4/js/toggle-labs.js?20241022" type="text/javascript"></script> <script src="/static/browse/0.3.4/js/cite.js" type="text/javascript"></script><meta name="citation_title" content="Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars" /><meta name="citation_author" content="von Forstner, Johan L. Freiherr" /><meta name="citation_author" content="Guo, Jingnan" /><meta name="citation_author" content="Wimmer-Schweingruber, Robert F." /><meta name="citation_author" content="Hassler, Donald M." /><meta name="citation_author" content="Temmer, Manuela" /><meta name="citation_author" content="Dumbovi膰, Mateja" /><meta name="citation_author" content="Jian, Lan K." /><meta name="citation_author" content="Appel, Jan K." /><meta name="citation_author" content="膶alogovi膰, Ja拧a" /><meta name="citation_author" content="Ehresmann, Bent" /><meta name="citation_author" content="Heber, Bernd" /><meta name="citation_author" content="Lohf, Henning" /><meta name="citation_author" content="Posner, Arik" /><meta name="citation_author" content="Steigies, Christian T." /><meta name="citation_author" content="Vr拧nak, Bojan" /><meta name="citation_author" content="Zeitlin, Cary J." /><meta name="citation_doi" content="10.1002/2017JA024700" /><meta name="citation_date" content="2017/12/19" /><meta name="citation_online_date" content="2017/12/19" /><meta name="citation_pdf_url" content="http://arxiv.org/pdf/1712.07301" /><meta name="citation_arxiv_id" content="1712.07301" /><meta name="citation_abstract" content="The propagation of 15 interplanetary coronal mass ejections (ICMEs) from Earth's orbit (1 AU) to Mars (~ 1.5 AU) has been studied with their propagation speed estimated from both measurements and simulations. The enhancement of magnetic fields related to ICMEs and their shock fronts cause the so-called Forbush decrease, which can be de- tected as a reduction of galactic cosmic rays measured on-ground. We have used galactic cosmic ray (GCR) data from in-situ measurements at Earth, from both STEREO A and B as well as GCR measurements by the Radiation Assessment Detector (RAD) instrument onboard Mars Science Laboratory (MSL) on the surface of Mars. A set of ICME events has been selected during the periods when Earth (or STEREO A or B) and Mars locations were nearly aligned on the same side of the Sun in the ecliptic plane (so-called opposition phase). Such lineups allow us to estimate the ICMEs' transit times between 1 and 1.5 AU by estimating the delay time of the corresponding Forbush decreases measured at each location. We investigate the evolution of their propagation speeds before and after passing Earth's orbit and find that the deceleration of ICMEs due to their interaction with the ambient solar wind may continue beyond 1 AU. We also find a substantial variance of the speed evolution among different events revealing the dynamic and diverse nature of eruptive solar events. Furthermore, the results are compared to simulation data obtained from two CME propagation models, namely the Drag-Based Model and ENLIL plus cone model." /> </head> <body class="with-cu-identity"> <aside class="slider-wrapper bps-banner forum blue"> <div class="columns"> <img role="presentation" class="bps-banner-image" src="/static/browse/0.3.4/images/icons/HF-Smiley-Bones-Banner.png" alt="arXiv smile and hugging face"> <div class="copy-donation bps-banner"> <h2>Support arXiv on Giving Day with Hugging Face!</h2> <p>Today Hugging Face is TRIPLING your donation to arXiv with a 2:1 match! 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href="https://arxiv.org/search/physics?searchtype=author&query=von+Forstner,+J+L+F" rel="nofollow">Johan L. Freiherr von Forstner</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Guo,+J" rel="nofollow">Jingnan Guo</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Wimmer-Schweingruber,+R+F" rel="nofollow">Robert F. Wimmer-Schweingruber</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Hassler,+D+M" rel="nofollow">Donald M. Hassler</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Temmer,+M" rel="nofollow">Manuela Temmer</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Dumbovi%C4%87,+M" rel="nofollow">Mateja Dumbovi膰</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Jian,+L+K" rel="nofollow">Lan K. Jian</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Appel,+J+K" rel="nofollow">Jan K. Appel</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=%C4%8Calogovi%C4%87,+J" rel="nofollow">Ja拧a 膶alogovi膰</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Ehresmann,+B" rel="nofollow">Bent Ehresmann</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Heber,+B" rel="nofollow">Bernd Heber</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Lohf,+H" rel="nofollow">Henning Lohf</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Posner,+A" rel="nofollow">Arik Posner</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Steigies,+C+T" rel="nofollow">Christian T. Steigies</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Vr%C5%A1nak,+B" rel="nofollow">Bojan Vr拧nak</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Zeitlin,+C+J" rel="nofollow">Cary J. Zeitlin</a></div> <div id="download-button-info" hidden>View a PDF of the paper titled Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars, by Johan L. Freiherr von Forstner and 15 other authors</div> <a class="mobile-submission-download" href="/pdf/1712.07301">View PDF</a> <blockquote class="abstract mathjax"> <span class="descriptor">Abstract:</span>The propagation of 15 interplanetary coronal mass ejections (ICMEs) from Earth's orbit (1 AU) to Mars (~ 1.5 AU) has been studied with their propagation speed estimated from both measurements and simulations. The enhancement of magnetic fields related to ICMEs and their shock fronts cause the so-called Forbush decrease, which can be de- tected as a reduction of galactic cosmic rays measured on-ground. We have used galactic cosmic ray (GCR) data from in-situ measurements at Earth, from both STEREO A and B as well as GCR measurements by the Radiation Assessment Detector (RAD) instrument onboard Mars Science Laboratory (MSL) on the surface of Mars. A set of ICME events has been selected during the periods when Earth (or STEREO A or B) and Mars locations were nearly aligned on the same side of the Sun in the ecliptic plane (so-called opposition phase). Such lineups allow us to estimate the ICMEs' transit times between 1 and 1.5 AU by estimating the delay time of the corresponding Forbush decreases measured at each location. We investigate the evolution of their propagation speeds before and after passing Earth's orbit and find that the deceleration of ICMEs due to their interaction with the ambient solar wind may continue beyond 1 AU. We also find a substantial variance of the speed evolution among different events revealing the dynamic and diverse nature of eruptive solar events. Furthermore, the results are compared to simulation data obtained from two CME propagation models, namely the Drag-Based Model and ENLIL plus cone model. </blockquote>  <div class="metatable"> <table summary="Additional metadata"><tr> <td class="tablecell label">Subjects:</td> <td class="tablecell subjects"> <span class="primary-subject">Space Physics (physics.space-ph)</span>; Solar and Stellar Astrophysics (astro-ph.SR)</td> </tr><tr> <td class="tablecell label">Cite as:</td> <td class="tablecell arxivid"><span class="arxivid"><a href="https://arxiv.org/abs/1712.07301">arXiv:1712.07301</a> [physics.space-ph]</span></td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxividv">(or <span class="arxivid"> <a href="https://arxiv.org/abs/1712.07301v1">arXiv:1712.07301v1</a> [physics.space-ph]</span> for this version) </td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxivdoi"> <a href="https://doi.org/10.48550/arXiv.1712.07301" id="arxiv-doi-link">https://doi.org/10.48550/arXiv.1712.07301</a><div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> arXiv-issued DOI via DataCite</div> </div> </td> </tr> <tr> <td class="tablecell label"> <abbr title="Digital Object Identifier">Related DOI</abbr>: </td> <td class="tablecell doi"><a href="https://doi.org/10.1002/2017JA024700" data-doi="10.1002/2017JA024700" class="link-https link-external" rel="external noopener nofollow">https://doi.org/10.1002/2017JA024700</a>  <div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> DOI(s) linking to related resources </div> </div> </td> </tr> </table> </div> </div> </div> <div class="submission-history"> <h2>Submission history</h2> From: Jingnan Guo Dr. [<a href="/show-email/c202b60a/1712.07301" rel="nofollow">view email</a>] <br/> <strong>[v1]</strong> Tue, 19 Dec 2017 12:34:20 UTC (5,437 KB)<br/> </div> </div>  <div class="extra-services"> <div class="full-text"> <a name="other"></a> <span class="descriptor">Full-text links:</span> <h2>Access Paper:</h2> <ul> <div id="download-button-info" hidden> View a PDF of the paper titled Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars, by Johan L. 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[1712.07301] Using Forbush decreases to derive the transit time of ICMEs propagating from 1 AU to Mars