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  • Journal article
    Khotyaintsev Y, Graham DB, Vaivads A, Steinvall K, Edberg NJT, Eriksson A, Johansson EPG, Sorriso-Valvo L, Maksimovic M, Bale SD, Chust T, Krasnoselskikh V, Kretzschmar M, Lorfevre E, Plettemeier D, Soucek J, Steller M, Stverak S, Travnicek P, Vecchio A, Horbury TS, O'Brien H, Evans V, Angelini V, Lorfevre Eet al., 2021,

    Density fluctuations associated with turbulence and waves First observations by Solar Orbiter

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Weiss AJ, Moestl C, Davies EE, Amerstorfer T, Bauer M, Hinterreiter J, Reiss MA, Bailey RL, Horbury TS, O'Brien H, Evans V, Angelini V, Heyner D, Richter I, Auster H-U, Magnes W, Fischer D, Baumjohann Wet al., 2021,

    Multi-point analysis of coronal mass ejection flux ropes using combined data from Solar Orbiter, BepiColombo, and Wind

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Eastwood JP, Stawarz JE, Phan TD, Laker R, Robertson S, Zhao L-L, Zank GP, Lavraud B, Shay MA, Evans V, Angelini V, O'Brien H, Horbury TSet al., 2021,

    Solar Orbiter observations of an ion-scale flux rope confined to a bifurcated solar wind current sheet

    , Astronomy & Astrophysics, Vol: 656, Pages: 1-8, ISSN: 0004-6361

    Context. Flux ropes in the solar wind are a key element of heliospheric dynamics and particle acceleration. When associated withcurrent sheets, the primary formation mechanism is magnetic reconnection and flux ropes in current sheets are commonly used astracers of the reconnection process.Aims. Whilst flux ropes associated with reconnecting current sheets in the solar wind have been reported, their occurrence, sizedistribution, and lifetime are not well understood.Methods. Here we present and analyse new Solar Orbiter magnetic field data reporting novel observations of a flux rope confined toa bifurcated current sheet in the solar wind. Comparative data and large-scale context is provided by Wind.Results. The Solar Orbiter observations reveal that the flux rope, which does not span the current sheet, is of ion scale, and in areconnection formation scenario, existed for a prolonged period of time as it was carried out in the reconnection exhaust. Wind is alsofound to have observed clear signatures of reconnection at what may be the same current sheet, thus demonstrating that reconnectionsignatures can be found separated by as much as ∼ 2 000 Earth radii, or 0.08 au.Conclusions. The Solar Orbiter observations provide new insight into the hierarchy of scales on which flux ropes can form, and showthat they exist down to the ion scale in the solar wind. The context provided by Wind extends the spatial scale over which reconnectionsignatures have been found at solar wind current sheets. The data suggest the local orientations of the current sheet at Solar Orbiterand Wind are rotated relative to each other, unlike reconnection observed at smaller separations; the implications of this are discussedwith reference to patchy vs. continuous reconnection scenarios.
  • Journal article
    Lavraud B, Kieokaew R, Fargette N, Louarn P, Fedorov A, André N, Fruit G, Génot V, Réville V, Rouillard AP, Plotnikov I, Penou E, Barthe A, Prech L, Owen CJ, Bruno R, Allegrini F, Berthomier M, Kataria D, Livi S, Raines JM, D'Amicis R, Eastwood JP, Froment C, Laker R, Maksimovic M, Marcucci F, Perri S, Perrone D, Phan TD, Stansby D, Stawarz J, Redondo ST, Vaivads A, Verscharen D, Zouganelis I, Angelini V, Evans V, Horbury TS, O'brien Het al., 2021,

    Magnetic reconnection as a mechanism to produce multiple protonpopulations and beams locally in the solar wind

    , Journal of Astrophysics and Astronomy, Vol: 656, Pages: 1-8, ISSN: 0250-6335

    Context. Spacecraft observations early revealed frequent multiple protonpopulations in the solar wind. Decades of research on their origin have focusedon processes such as magnetic reconnection in the low corona and wave-particleinteractions in the corona and locally in the solar wind.Aims.This study aimsto highlight that multiple proton populations and beams are also produced bymagnetic reconnection occurring locally in the solar wind. Methods. We use highresolution Solar Orbiter proton velocity distribution function measurements,complemented by electron and magnetic field data, to analyze the association ofmultiple proton populations and beams with magnetic reconnection during aperiod of slow Alfv\'enic solar wind on 16 July 2020. Results. At least 6reconnecting current sheets with associated multiple proton populations andbeams, including a case of magnetic reconnection at a switchback boundary, arefound during this day. This represents 2% of the measured distributionfunctions. We discuss how this proportion may be underestimated, and how it maydepend on solar wind type and distance from the Sun. Conclusions. Althoughsuggesting a likely small contribution, but which remains to be quantitativelyassessed, Solar Orbiter observations show that magnetic reconnection must beconsidered as one of the mechanisms that produce multiple proton populationsand beams locally in the solar wind.
  • Journal article
    Wimmer-Schweingruber RF, Janitzek NP, Pacheco D, Cernuda I, Lara FE, Gomez-Herrero R, Mason GM, Allen RC, Xu ZG, Carcaboso F, Kollhoff A, Kuehl P, von Forstner JLF, Berger L, Rodriguez-Pacheco J, Ho GC, Andrews GB, Angelini V, Aran A, Boden S, Bottcher S, Carrasco A, Dresing N, Eldrum S, Elftmann R, Evans V, Gevin O, Hayes J, Heber B, Horbury TS, Kulkarni SR, Lario D, Lees WJ, Limousin O, Malandraki OE, Martin C, O'Brien H, Mateo MP, Ravanbakhsh A, Rodriguez-Polo O, Sanchez Prieto S, Schlemm CE, Seifert H, Terasa JC, Tyagi K, Vainio R, Walsh A, Yedla MKet al., 2021,

    First year of energetic particle measurements in the inner heliosphere with Solar Orbiter's Energetic Particle Detector

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Kasper JC, Klein KG, Lichko E, Huang J, Chen CHK, Badman ST, Bonnell J, Whittlesey PL, Livi R, Larson D, Pulupa M, Rahmati A, Stansby D, Korreck KE, Stevens M, Case AW, Bale SD, Maksimovic M, Moncuquet M, Goetz K, Halekas JS, Malaspina D, Raouafi NE, Szabo A, MacDowall R, Velli M, de Wit TD, Zank GPet al., 2021,

    <i>Parker</i><i> Solar</i><i> Probe</i> Enters the Magnetically Dominated Solar Corona

    , PHYSICAL REVIEW LETTERS, Vol: 127, ISSN: 0031-9007
  • Journal article
    Vecchio A, Maksimovic M, Krupar V, Bonnin X, Zaslavsky A, Astier PL, Dekkali M, Cecconi B, Bale SD, Chust T, Guilhem E, Khotyaintsev Y, Krasnoselskikh V, Kretzschmar M, Lorfevre E, Plettemeier D, Souceck J, Steller M, Stverak S, Travnicek P, Vaivads Aet al., 2021,

    Solar Orbiter/RPW antenna calibration in the radio domain and its application to type III burst observations

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Musset S, Maksimovic M, Kontar E, Krupar V, Chrysaphi N, Bonnin X, Vecchio A, Cecconi B, Zaslavsky A, Issautier K, Bale SD, Pulupa Met al., 2021,

    Simulations of radio-wave anisotropic scattering to interpret type III radio burst data from Solar Orbiter, Parker Solar Probe, STEREO, and Wind

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Soucek J, Pisa D, Kolmasova I, Uhlir L, Lan R, Santolik O, Krupar V, Kruparova O, Base J, Maksimovic M, Bale SD, Chust T, Khotyaintsev Y, Krasnoselskikh V, Kretzschmar M, Lorfevre E, Plettemeier D, Steller M, Stverak S, Vaivads A, Vecchio A, Berard D, Bonnin Xet al., 2021,

    Solar Orbiter Radio and Plasma Waves - Time Domain Sampler: In-flight performance and first results

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Gomez-Herrero R, Pacheco D, Kollhoff A, Lara FE, von Forstner JLF, Dresing N, Lario D, Balmaceda L, Krupar V, Malandraki OE, Aran A, Bucik R, Klassen A, Klein K-L, Cernuda I, Eldrum S, Reid H, Mitchell JG, Mason GM, Ho GC, Rodriguez-Pacheco J, Wimmer-Schweingruber RF, Heber B, Berger L, Allen RC, Janitzek NP, Laurenza M, De Marco R, Wijsen N, Kartavykh YY, Droge W, Horbury TS, Maksimovic M, Owen CJ, Vecchio A, Bonnin X, Kruparova O, Pisa D, Soucek J, Louarn P, Fedorov A, O'Brien H, Evans V, Angelini V, Zucca P, Prieto M, Sanchez-Prieto S, Carrasco A, Blanco JJ, Parra P, Rodriguez-Polo O, Martin C, Terasa JC, Boden S, Kulkarni SR, Ravanbakhsh A, Yedla M, Xu Z, Andrews GB, Schlemm CE, Seifert H, Tyagi K, Lees WJ, Hayes Jet al., 2021,

    First near-relativistic solar electron events observed by EPD onboard Solar Orbiter

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Adhikari L, Zank GP, Zhao L-L, Telloni D, Horbury TS, O'Brien H, Evans V, Angelini V, Owen CJ, Louarn P, Fedorov Aet al., 2021,

    Evolution of anisotropic turbulence in the fast and slow solar wind: Theory and Solar Orbiter measurements

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Kretzschmar M, Chust T, Krasnoselskikh V, Graham D, Colomban L, Maksimovic M, Khotyaintsev Y, Soucek J, Steinvall K, Santolik O, Jannet G, Brochot J-Y, Le Contel O, Vecchio A, Bonnin X, Bale SD, Froment C, Larosa A, Bergerard-Timofeeva M, Fergeau P, Lorfevre E, Plettemeier D, Steller M, Stverak S, Travnicek P, Vaivads A, Horbury TS, O'Brien H, Evans V, Angelini V, Owen CJ, Louarn Pet al., 2021,

    Whistler waves observed by Solar Orbiter/RPW between 0.5 AU and 1 AU

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Owen CJ, Kataria DO, Bercic L, Horbury TS, Berthomier M, Verscharen D, Bruno R, Livi S, Louarn P, Anekallu C, Kelly CW, Lewis GR, Watson G, Fortunato V, Mele G, Nicolaou G, Wicks RT, O'Brien H, Evans V, Angelini Vet al., 2021,

    High-cadence measurements of electron pitch-angle distributions from Solar Orbiter SWA-EAS burst mode operations

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Kilpua EKJ, Good SW, Dresing N, Vainio R, Davies EE, Forsyth RJ, Gieseler J, Lavraud B, Asvestari E, Morosan DE, Pomoell J, Price DJ, Heyner D, Horbury TS, Angelini V, O'Brien H, Evans V, Rodriguez-Pacheco J, Herrero RG, Ho GC, Wimmer-Schweingruber Ret al., 2021,

    Multi-spacecraft observations of the structure of the sheath of an interplanetary coronal mass ejection and related energetic ion enhancement

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Maksimovic M, Soucek J, Chust T, Khotyaintsev Y, Kretzschmar M, Bonnin X, Vecchio A, Alexandrova O, Bale SD, Berard D, Brochot J-Y, Edberg NJT, Eriksson A, Hadid LZ, Johansson EPG, Karlsson T, Katra B, Krasnoselskikh V, Krupar V, Lion S, Lorfevre E, Matteini L, Nguyen QN, Pisa D, Piberne R, Plettemeier D, Rucker HO, Santolik O, Steinvall K, Steller M, Stverak S, Travnicek P, Vaivads A, Zaslavsky A, Chaintreuil S, Dekkali M, Astier P-A, Barbary G, Boughedada K, Cecconi B, Chapron F, Collin C, Dias D, Gueguen L, Lamy L, Leray V, Malac-Allain LR, Pantellini F, Parisot J, Plasson P, Thijs S, Fratter I, Bellouard E, Danto P, Julien S, Guilhem E, Fiachetti C, Sanisidro J, Laffaye C, Gonzalez F, Pontet B, Queruel N, Jannet G, Fergeau P, de Wit TD, Vincent T, Agrapart C, Pragout J, Bergerard-Timofeeva M, Delory GT, Turin P, Jeandet A, Leroy P, Pellion J-C, Bouzid V, Recart W, Kolmasova I, Kruparova O, Uhlir L, Lan R, Base J, Andre M, Bylander L, Cripps V, Cully C, Jansson S-E, Puccio W, Brinek J, Ottacher H, Angelini V, Berthomier M, Evans V, Goetz K, Hellinger P, Horbury TS, Issautier K, Kontar E, Le Contel O, Louarn P, Martinovic M, Mueller D, O'Brien H, Owen CJ, Retino A, Rodriguez-Pacheco J, Sahraoui F, Sanchez L, Walsh AP, Wimmer-Schweingruber RF, Zouganelis Iet al., 2021,

    First observations and performance of the RPW instrument on board the Solar Orbiter mission

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Telloni D, Scolini C, Moestl C, Zank GP, Zhao L-L, Weiss AJ, Reiss MA, Laker R, Perrone D, Khotyaintsev Y, Steinvall K, Sorriso-Valvo L, Horbury TS, Wimmer-Schweingruber RF, Bruno R, D'Amicis R, De Marco R, Jagarlamudi VK, Carbone F, Marino R, Stangalini M, Nakanotani M, Adhikari L, Liang H, Woodham LD, Davies EE, Hietala H, Perri S, Gomez-Herrero R, Rodriguez-Pacheco J, Antonucci E, Romoli M, Fineschi S, Maksimovic M, Soucek J, Chust T, Kretzschmar M, Vecchio A, Muller D, Zouganelis I, Winslow RM, Giordano S, Mancuso S, Susino R, Ivanovski SL, Messerotti M, O'Brien H, Evans V, Angelini Vet al., 2021,

    Study of two interacting interplanetary coronal mass ejections encountered by Solar Orbiter during its first perihelion passage Observations and modeling

    , Astronomy and Astrophysics: a European journal, Vol: 656, ISSN: 0004-6361

    Context. Solar Orbiter, the new-generation mission dedicated to solar and heliospheric exploration, was successfully launched on February 10, 2020, 04:03 UTC from Cape Canaveral. During its first perihelion passage in June 2020, two successive interplanetary coronal mass ejections (ICMEs), propagating along the heliospheric current sheet (HCS), impacted the spacecraft.Aims. This paper addresses the investigation of the ICMEs encountered by Solar Orbiter on June 7−8, 2020, from both an observational and a modeling perspective. The aim is to provide a full description of those events, their mutual interaction, and their coupling with the ambient solar wind and the HCS.Methods. Data acquired by the MAG magnetometer, the Energetic Particle Detector suite, and the Radio and Plasma Waves instrument are used to provide information on the ICMEs’ magnetic topology configuration, their magnetic connectivity to the Sun, and insights into the heliospheric plasma environment where they travel, respectively. On the modeling side, the Heliospheric Upwind eXtrapolation model, the 3D COronal Rope Ejection technique, and the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) tool are used to complement Solar Orbiter observations of the ambient solar wind and ICMEs, and to simulate the evolution and interaction of the ejecta in the inner heliosphere, respectively.Results. Both data analysis and numerical simulations indicate that the passage of two distinct, dynamically and magnetically interacting (via magnetic reconnection processes) ICMEs at Solar Orbiter is a possible scenario, supported by the numerous similarities between EUHFORIA time series at Solar Orbiter and Solar Orbiter data.Conclusions. The combination of in situ measurements and numerical simulations (together with remote sensing observations of the corona and inner heliosphere) will significantly lead to a deeper understanding of the physical processes occurring during the CME-CME interaction.
  • Journal article
    Hadid LZ, Edberg NJT, Chust T, Pisa D, Dimmock AP, Morooka MW, Maksimovic M, Khotyaintsev Y, Soucek J, Kretzschmar M, Vecchio A, Le Contel O, Retino A, Allen RC, Volwerk M, Fowler CM, Sorriso-Valvo L, Karlsson T, Santolik O, Kolmasova I, Sahraoui F, Stergiopoulou K, Moussas X, Issautier K, Dewey RM, Wolt MK, Malandraki OE, Kontar EP, Howes GG, Bale SD, Horbury TS, Martinovic M, Vaivads A, Krasnoselskikh V, Lorfevre E, Plettemeier D, Steller M, Stverak S, Travnicek P, O'Brien H, Evans V, Angelini V, Velli MC, Zouganelis Iet al., 2021,

    Solar Orbiter's first Venus flyby: Observations from the Radio and Plasma Wave instrument

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Kollhoff A, Kouloumvakos A, Lario D, Dresing N, Gomez-Herrero R, Rodriguez-Garcia L, Malandraki OE, Richardson IG, Posner A, Klein K-L, Pacheco D, Klassen A, Heber B, Cohen CMS, Laitinen T, Cernuda I, Dalla S, Lara FE, Vainio R, Koeberle M, Kuehl R, Xu ZG, Berger L, Eldrum S, Bruedern M, Laurenza M, Kilpua EJ, Aran A, Rouillard AP, Bucik R, Wijsen N, Pomoell J, Wimmer-Schweingruber RF, Martin C, Boettcher S, von Forstner JLF, Terasa J-C, Boden S, Kulkarni SR, Ravanbakhsh A, Yedla M, Janitzek N, Rodriguez-Pacheco J, Mateo MP, Prieto SS, Espada PP, Polo OR, Hellin AM, Carcaboso F, Mason GM, Ho GC, Allen RC, Andrews GB, Schlemm CE, Seifert H, Tyagi K, Lees WJ, Hayes J, Bale SD, Krupar V, Horbury TS, Angelini V, Evans V, O'Brien H, Maksimovic M, Khotyaintsev Y, Vecchio A, Steinvall K, Asvestari Eet al., 2021,

    The first widespread solar energetic particle event observed by Solar Orbiter on 2020 November 29

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    D'Amicis R, Bruno R, Panasenco O, Telloni D, Perrone D, Marcucci MF, Woodham L, Velli M, De Marco R, Jagarlamudi V, Coco I, Owen C, Louarn P, Livi S, Horbury T, Andre N, Angelini V, Evans V, Fedorov A, Genot V, Lavraud B, Matteini L, Muller D, O'Brien H, Pezzi O, Rouillard AP, Sorriso-Valvo L, Tenerani A, Verscharen D, Zouganelis Iet al., 2021,

    First Solar Orbiter observation of the Alfvenic slow wind and identification of its solar source

    , Astronomy and Astrophysics: a European journal, Vol: 656, Pages: 1-17, ISSN: 0004-6361

    Context. Turbulence dominated by large-amplitude, nonlinear Alfvén-like fluctuations mainly propagating away from the Sun is ubiquitous in high-speed solar wind streams. Recent studies have demontrated that slow wind streams may also show strong Alfvénic signatures, especially in the inner heliosphere.Aims. The present study focuses on the characterisation of an Alfvénic slow solar wind interval observed by Solar Orbiter between 14 and 18 July 2020 at a heliocentric distance of 0.64 AU.Methods. Our analysis is based on plasma moments and magnetic field measurements from the Solar Wind Analyser (SWA) and Magnetometer (MAG) instruments, respectively. We compared the behaviour of different parameters to characterise the stream in terms of the Alfvénic content and magnetic properties. We also performed a spectral analysis to highlight spectral features and waves signature using power spectral density and magnetic helicity spectrograms, respectively. Moreover, we reconstruct the Solar Orbiter magnetic connectivity to the solar sources both via a ballistic and a potential field source surface (PFSS) model.Results. The Alfvénic slow wind stream described in this paper resembles, in many respects, a fast wind stream. Indeed, at large scales, the time series of the speed profile shows a compression region, a main portion of the stream, and a rarefaction region, characterised by different features. Moreover, before the rarefaction region, we pinpoint several structures at different scales recalling the spaghetti-like flux-tube texture of the interplanetary magnetic field. Finally, we identify the connections between Solar Orbiter in situ measurements, tracing them down to coronal streamer and pseudostreamer configurations.Conclusions. The characterisation of the Alfvénic slow wind stream observed by Solar Orbiter and the identification of its solar source are extremely important aspects for improving the understanding of future observ
  • Journal article
    von Forstner JLF, Dumbovi M, Moestl C, Guo J, Papaioannou A, Elftmann R, Xu Z, Terasa JC, Kollhoff A, Wimmer-Schweingruber RF, Rodriguez-Pacheco J, Weiss AJ, Hinterreiter J, Amerstorfer T, Bauer M, Belov A, Abunina MA, Horbury T, Davies EE, O'Brien H, Allen RC, Andrews GB, Berger L, Boden S, Cernuda Cangas I, Eldrum S, Espinosa Lara F, Gomez Herrero R, Hayes JR, Ho GC, Kulkarni SR, Lees WJ, Martin C, Mason GM, Pacheco D, Prieto Mateo M, Ravanbakhsh A, Rodriguez Polo O, Sanchez Prieto S, Schlemm CE, Seifert H, Tyagi K, Yedla Met al., 2021,

    Radial evolution of the April 2020 stealth coronal mass ejection between 0.8 and 1AU Comparison of Forbush decreases at Solar Orbiter and near the Earth

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Owen CJ, Foster AC, Bruno R, Livi S, Louarn P, Berthomier M, Fedorov A, Anekallu C, Kataria D, Kelly CW, Lewis GR, Watson G, Bercic L, Stansby D, Suen G, Verscharen D, Fortunato V, Nicolaou G, Wicks RT, Rae IJ, Lavraud B, Horbury TS, O'Brien H, Evans V, Angelini Vet al., 2021,

    Solar Orbiter observations of the structure of reconnection outflow layers in the solar wind

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Fedorov A, Louarn P, Owen CJ, Horbury TS, Prech L, Durovcova T, Barthe A, Rouillard AP, Kasper JC, Bale SD, Bruno R, O'Brien H, Evans V, Angelini V, Larson D, Livi R, Lavraud B, Andre N, Genot V, Penou E, Mele G, Fortunato Vet al., 2021,

    Switchback-like structures observed by Solar Orbiter

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Chust T, Kretzschmar M, Graham DB, Le Contel O, Retino A, Alexandrova A, Berthomier M, Hadid LZ, Sahraoui F, Jeandet A, Leroy P, Pellion J-C, Bouzid V, Katra B, Piberne R, Khotyaintsev Y, Vaivads A, Krasnoselskikh V, Soucek J, Santolik O, Lorfevre E, Plettemeier D, Steller M, Stverak S, Vecchio A, Maksimovic M, Bale SD, Horbury TS, O'Brien H, Evans V, Angelini Vet al., 2021,

    Observations of whistler mode waves by Solar Orbiter's RPW Low Frequency Receiver (LFR): In-flight performance and first results

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Aran A, Pacheco D, Laurenza M, Wijsen N, Lario D, Benella S, Richardson IG, Samara E, von Forstner JLF, Sanahuja B, Rodriguez L, Balmaceda L, Lara FE, Gomez-Herrero R, Steinvall K, Vecchio A, Krupar V, Poedts S, Allen RC, Andrews GB, Angelini V, Berger L, Berghmans D, Boden S, Bottcher S, Carcaboso F, Cernuda I, De Marco R, Eldrum S, Evans V, Fedorov A, Hayes J, Ho GC, Horbury TS, Janitzek NP, Khotyaintsev Y, Kollhoff A, Kuehl P, Kulkarni SR, Lees WJ, Louarn P, Magdalenic J, Maksimovic M, Malandraki O, Martinez A, Mason GM, Martin C, O'Brien H, Owen C, Parra P, Prieto Mateo M, Ravanbakhsh A, Rodriguez-Pacheco J, Rodriguez Polo O, Sanchez Prieto S, Schlemm CE, Seifert H, Terasa JC, Tyagi K, Verbeeck C, Wimmer-Schweingruber RF, Xu ZG, Yedla MK, Zhukov ANet al., 2021,

    Evidence for local particle acceleration in the first recurrent galactic cosmic ray depression observed by Solar Orbiter The ion event on 19 June 2020

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Louarn P, Fedorov A, Prech L, Owen CJ, Bruno R, Livi S, Lavraud B, Rouillard AP, Genot V, Andre N, Fruit G, Reville V, Kieokaew R, Plotnikov I, Penou E, Barthe A, Khataria D, Berthomier M, D'Amicis R, Sorriso-Valvo L, Allegrini F, Raines J, Verscharen D, Fortunato V, Mele G, Horbury TS, O'brien H, Evans V, Angelini V, Maksimovic M, Kasper JC, Bale SDet al., 2021,

    Multiscale views of an Alfvenic slow solar wind: 3D velocity distribution functions observed by the Proton-Alpha Sensor of Solar Orbiter

    , ASTRONOMY & ASTROPHYSICS, Vol: 656, ISSN: 0004-6361
  • Journal article
    Cargill PJ, Bradshaw SJ, Klimchuk JA, Barnes WTet al., 2021,

    Static and dynamic solar coronal loops with cross-sectional area variations

    , Monthly Notices of the Royal Astronomical Society, Vol: 509, Pages: 4420-4429, ISSN: 0035-8711

    The Enthalpy Based Thermal Evolution of Loops approximate model for static and dynamic coronal loops is developed to include the effect of a loop cross-sectional area which increases from the base of the transition region (TR) to the corona. The TR is defined as the part of a loop between the top of the chromosphere and the location where thermal conduction changes from an energy loss to an energy gain. There are significant differences from constant area loops due to the manner in which the reduced volume of the TR responds to conductive and enthalpy fluxes from the corona. For static loops with modest area variation the standard picture of loop energy balance is retained, with the corona and TR being primarily a balance between heating and conductive losses in the corona, and downward conduction and radiation to space in the TR. As the area at the loop apex increases, the TR becomes thicker and the density in TR and corona larger. For large apex areas, the coronal energy balance changes to one primarily between heating and radiation, with conduction playing an increasingly unimportant role, and the TR thickness becoming a significant fraction of the loop length. Approximate scaling laws are derived that give agreement with full numerical solutions for the density, but not the temperature. For non-uniform areas, dynamic loops have a higher peak temperature and are denser in the radiative cooling phase by of order 50 per cent than the constant area case for the examples considered. They also show a final rapid cooling and draining once the temperature approaches 1 MK. Although the magnitude of the emission measure will be enhanced in the radiative phase, there is little change in the important observational diagnostic of its temperature dependence.
  • Journal article
    Schwartz S, Kucharek H, Farrugia C, Trattner K, Gingell I, Chasapis A, Gershman D, Strangeway Ret al., 2021,

    Characteristics of Intense Current-carrying Structures in the Terrestrial Magnetosheath
  • Journal article
    Cochrane CJ, Vance SD, Nordheim TA, Styczinski M, Masters A, Regoli LHet al., 2021,

    In search of subsurface oceans within the Uranian moons

    , Journal of Geophysical Research: Planets, Vol: 126, ISSN: 2169-9097

    The Galileo mission to Jupiter discovered magnetic signatures associated with hidden sub-surface oceans at the moons Europa and Callisto using the phenomenon of magnetic induction. These induced magnetic fields originate from electrically conductive layers within the moons and are driven by Jupiter’s strong time-varying magnetic field. The ice giants and their moons are also ideal laboratories for magnetic induction studies. Both Uranus and Neptune have a strongly tilted magnetic axis with respect to their spin axis, creating a dynamic and strongly variable magnetic field environment at the orbits of their major moons. Although Voyager-2 visited the ice giants in the 1980s, it did not pass close enough to any of the moons to detect magnetic induction signatures. However, Voyager-2 revealed that some of these moons exhibit surface features that hint at recent geologically activity, possibly associated with sub-surface oceans. Future missions to the ice giants may therefore be capable of discovering sub-surface oceans, thereby adding to the family of known “ocean worlds” in our solar system. Here, we assess magnetic induction as a technique for investigating sub-surface oceans within the major moons of Uranus. Furthermore, we establish the ability to distinguish induction responses created by different interior characteristics that tie into the induction response: ocean thickness, conductivity, and depth, and ionospheric conductance. The results reported here demonstrate the possibility of single-pass ocean detection and constrained characterization within the moons of Miranda, Ariel, and Umbriel, and provide guidance for magnetometer selection and trajectory design for future missions to Uranus.
  • Journal article
    Volwerk M, Horbury TS, Woodham LD, Bale SD, Simon Wedlund C, Schmid D, Allen RC, Angelini V, Baumjohann W, Berger L, Edberg NJT, Evans V, Hadid LZ, Ho GC, Khotyaintsev YV, Magnes W, Maksimovic M, OBrien H, Steller MB, Rodriguez-Pacheco J, Wimmer-Scheingruber RFet al., 2021,

    Solar Orbiter’s first Venus flyby. MAG observations of structures and waves associated with the induced Venusian magnetosphere

    , Astronomy and Astrophysics: a European journal, Vol: 656, ISSN: 0004-6361

    Context. The induced magnetosphere of Venus is caused by the interaction of the solar wind and embedded interplanetary magnetic field with the exosphere and ionosphere of Venus. Solar Orbiter entered Venus’s magnetotail far downstream, > 70 Venus radii, of the planet and exited the magnetosphere over the north pole. This offered a unique view of the system over distances that had only been flown through before by three other missions, Mariner 10, Galileo, and BepiColombo.Aims. In this study, we study the large-scale structure and activity of the induced magnetosphere as well as the high-frequency plasma waves both in the magnetosphere and in a limited region upstream of the planet where interaction with Venus’s exosphere is expected.Methods. The large-scale structure of the magnetosphere was studied with low-pass filtered data and identified events are investigated with a minimum variance analysis as well as combined with plasma data. The high-frequency plasma waves were studied with spectral analysis.Results. We find that Venus’s magnetotail is very active during the Solar Orbiter flyby. Structures such as flux ropes and reconnection sites were encountered, in addition to a strong overdraping of the magnetic field downstream of the bow shock and planet. High-frequency plasma waves (up to six times the local proton cyclotron frequency) are observed in the magnetotail, which are identified as Doppler-shifted proton cyclotron waves, whereas in the upstream solar wind, these waves appear just below the proton cyclotron frequency (as expected) but are very patchy. The bow shock is quasi-perpendicular, however, expected mirror mode activity is not found directly behind it; instead, there is strong cyclotron wave power. This is most likely caused by the relatively low plasma-β behind the bow shock. Much further downstream, magnetic hole or mirror mode structures are identified in the magnetosheath.
  • Journal article
    Bale SD, Horbury TS, Velli M, Desai MI, Halekas JS, McManus MD, Panasenco O, Badman ST, Bowen TA, Chandran BDG, Drake JF, Kasper JC, Laker R, Mallet A, Matteini L, Phan TD, Raouafi NE, Squire J, Woodham LD, Woolley Tet al., 2021,

    A solar source of alfvenic magnetic field switchbacks: in situ remnants of magnetic funnels on supergranulation scales

    , The Astrophysical Journal: an international review of astronomy and astronomical physics, Vol: 923, Pages: 1-12, ISSN: 0004-637X

    One of the striking observations from the Parker Solar Probe (PSP) spacecraft is the prevalence in the inner heliosphere of large amplitude, Alfvénic magnetic field reversals termed switchbacks. These $\delta {B}_{R}/B\sim { \mathcal O }(1$) fluctuations occur over a range of timescales and in patches separated by intervals of quiet, radial magnetic field. We use measurements from PSP to demonstrate that patches of switchbacks are localized within the extensions of plasma structures originating at the base of the corona. These structures are characterized by an increase in alpha particle abundance, Mach number, plasma β and pressure, and by depletions in the magnetic field magnitude and electron temperature. These intervals are in pressure balance, implying stationary spatial structure, and the field depressions are consistent with overexpanded flux tubes. The structures are asymmetric in Carrington longitude with a steeper leading edge and a small (∼1°) edge of hotter plasma and enhanced magnetic field fluctuations. Some structures contain suprathermal ions to ∼85 keV that we argue are the energetic tail of the solar wind alpha population. The structures are separated in longitude by angular scales associated with supergranulation. This suggests that these switchbacks originate near the leading edge of the diverging magnetic field funnels associated with the network magnetic field—the primary wind sources. We propose an origin of the magnetic field switchbacks, hot plasma and suprathermals, alpha particles in interchange reconnection events just above the solar transition region and our measurements represent the extended regions of a turbulent outflow exhaust.

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