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  • Journal article
    Hanson ELM, Agapitov OV, Vasko IY, Mozer FS, Krasnoselskikh V, Bale SD, Avanov L, Khotyaintsev Y, Giles Bet al., 2020,

    Shock Drift Acceleration of Ions in an Interplanetary Shock Observed by <i>MMS</i>

    , ASTROPHYSICAL JOURNAL LETTERS, Vol: 891, ISSN: 2041-8205
  • Journal article
    Agiwal O, Hunt GJ, Dougherty MK, Cowley SWH, Provan Get al., 2020,

    Modeling the Temporal Variability in Saturn's Magnetotail Current Sheet From the Cassini F-ring Orbits

    , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 125, ISSN: 2169-9380
  • Journal article
    DAmicis R, Matteini L, Bruno R, Velli Met al., 2020,

    Large amplitude fluctuations in the alfvénic solar wind

    , Solar Physics, Vol: 295, Pages: 1-12, ISSN: 0038-0938

    Large amplitude fluctuations, often with characteristics reminiscent of large amplitude Alfvén waves propagating away from the Sun, are ubiquitous in the solar wind. Such features are most frequently found within fast solar wind streams and most often at solar minimum. The fluctuations found in slow solar wind streams usually have a smaller relative amplitude, are less Alfvénic in character and present more variability. However, intervals of slow wind displaying Alfvénic correlations have been recently identified in different solar cycle phases. In the present paper we report Alfvénic slow solar wind streams seen during the maximum of solar activity that are characterized not only by a very high correlation between velocity and magnetic field fluctuations (as required by outwardly propagating Alfvén modes) – comparable to that seen in fast wind streams – but also by higher amplitude relative fluctuations comparable to those seen in fast wind. Our results suggest that the Alfvénic slow wind has a different origin from the slow wind found near the boundary of coronal holes, where the amplitude of the Alfvénic fluctuations decreases together with decreasing the wind speed.
  • Journal article
    Bellouin N, Quaas J, Gryspeerdt E, Kinne S, Stier P, Watson-Parris D, Boucher O, Carslaw K, Christensen M, Daniau A-L, Dufresne J-L, Feingold G, Fiedler S, Forster P, Gettelman A, Haywood J, Lohmann U, Malavelle F, Mauritsen T, McCoy D, Myhre G, Mülmenstädt J, Neubauer D, Possner A, Rugenstein M, Sato Y, Schulz M, Schwartz S, Sourdeval O, Storelvmo T, Toll V, Winker D, Stevens Bet al., 2020,

    Bounding global aerosol radiative forcing of climate change

    , Reviews of Geophysics, Vol: 58, Pages: 1-45, ISSN: 8755-1209

    Aerosols interact with radiation and clouds. Substantial progress made over the past 40 years in observing, understanding, and modeling these processes helped quantify the im balance in the Earth’s radiation budget caused by anthropogenic aerosols, called aerosol radiative forcing, but uncertainties remain large. This review provides a new range of aerosol radiative forcing over the industrial era based on multiple, traceable and arguable lines of evidence, including modelling approaches, theoretical considerations, and obser vations. Improved understanding of aerosol absorption and the causes of trends in surface radiative fluxes constrain the forcing from aerosol-radiation interactions. A robust theoretical foundation and convincing evidence constrain the forcing caused by aerosol61 driven increases in liquid cloud droplet number concentration. However, the influence of anthropogenic aerosols on cloud liquid water content and cloud fraction is less clear, and the influence on mixed-phase and ice clouds remains poorly constrained. Observed changes in surface temperature and radiative fluxes provide additional constraints. These multiple lines of evidence lead to a 68% confidence interval for the total aerosol effective radiative forcing of −1.60 to −0.65 W m−2, or −2.0 to −0.4 W m−2 with a 90% like lihood. Those intervals are of similar width to the last Intergovernmental Panel on Cli mate Change assessment but shifted towards more negative values. The uncertainty will narrow in the future by continuing to critically combine multiple lines of evidence, especially those addressing industrial-era changes in aerosol sources and aerosol effects on liquid cloud amount and on ice clouds.
  • Journal article
    Lavergne A, Voelker S, Csank A, Graven H, de Boer HJ, Daux V, Robertson I, Dorado-Linan I, Martínez-Sancho E, Battipaglia G, Bloomfield KJ, Still C, Meinzer FC, Dawson TE, Camarero JJ, Clisby R, Fang Y, Menzel A, Keen RM, Roden JS, Prentice Iet al., 2020,

    Historical changes in the stomatal limitation of photosynthesis: empirical support for an optimality principle

    , New Phytologist, Vol: 225, Pages: 2484-2497, ISSN: 0028-646X

    The ratio of leaf‐internal (ci) to ambient (ca) partial pressure of CO2, defined here as χ, is an index of adjustments in both leaf stomatal conductance and photosynthetic rate to environmental conditions. Measurements and proxies of this ratio can be used to constrain vegetation models uncertainties for predicting terrestrial carbon uptake and water use.We test a theory based on the least‐cost optimality hypothesis for modelling historical changes in χ over the 1951‐2014 period, across different tree species and environmental conditions, as reconstructed from stable carbon isotopic measurements across a global network of 103 absolutely‐dated tree‐ring chronologies. The theory predicts optimal χ as a function of air temperature, vapour pressure deficit, ca and atmospheric pressure.The theoretical model predicts 39% of the variance in χ values across sites and years, but underestimates the inter‐site variability in the reconstructed χ trends, resulting in only 8% of the variance in χ trends across years explained by the model.Overall, our results support theoretical predictions that variations in χ are tightly regulated by the four environmental drivers. They also suggest that explicitly accounting for the effects of plant‐available soil water and other site‐specific characteristics might improve the predictions.
  • Journal article
    Haaland S, Paschmann G, Øieroset M, Phan T, Hasegawa H, Fuselier S, Constantinescu V, Eriksson S, Trattner KJ, Fadanelli S, Tenfjord P, Lavraud B, Norgren C, Eastwood JP, Hietala H, Burch Jet al., 2020,

    Characteristics of the flank magnetopause: MMS results

    , Journal of Geophysical Research: Space Physics, Vol: 125, Pages: 1-13, ISSN: 2169-9380

    We have used a large number of magnetopause crossings by the Magnetospheric Multi Spacecraft (MMS) mission to investigate macroscopic properties of this current sheet, with emphasis on the flanks of the magnetopause. Macroscopic features such as thickness, location and motion of the magnetopause were calculated as a function of local time sector. The results show that the flanks of the magnetopause are significantly thicker than the dayside magnetopause. Thicknesses vary from about 650 km near noon to over 1000 km near the terminator. Current densities varies in a similar manner, with average current densities around noon almost twice as high as near the terminator. We also find a dawn‐dusk asymmetry in many of the macroscopic parameters; The dawn magnetopause is thicker than at dusk, while the dusk flank is more dynamic, with a higher average normal velocity.
  • Journal article
    Simon AA, Fletcher LN, Arridge C, Atkinson D, Coustenis A, Ferri F, Hofstadter M, Masters A, Mousis O, Reh K, Turrini D, Witasse Oet al., 2020,

    A review of the in situ probe designs from recent ice giant mission concept studies

    , Space Science Reviews, Vol: 216, Pages: 1-13, ISSN: 0038-6308

    For the Ice Giants, atmospheric entry probes provide critical measurements not attainable via remote observations. Including the 2013–2022 NASA Planetary Decadal Survey, there have been at least five comprehensive atmospheric probe engineering design studies performed in recent years by NASA and ESA. International science definition teams have assessed the science requirements, and each recommended similar measurements and payloads to meet science goals with current instrument technology. The probe system concept has matured and converged on general design parameters that indicate the probe would include a 1-meter class aeroshell and have a mass around 350 to 400-kg. Probe battery sizes vary, depending on the duration of a post-release coast phase, and assumptions about heaters and instrument power needs. The various mission concepts demonstrate the need for advanced power and thermal protection system development. The many completed studies show an Ice Giant mission with an in situ probe is feasible and would be welcomed by the international science community.
  • Journal article
    Phan TD, Bale SD, Eastwood JP, Lavraud B, Drake JF, Oieroset M, Shay MA, Pulupa M, Stevens M, MacDowall RJ, Case AW, Larson D, Kasper J, Whittlesey P, Szabo A, Korreck KE, Bonnell JW, de Wit TD, Goetz K, Harvey PR, Horbury TS, Livi R, Malaspina D, Paulson K, Raouafi NE, Velli Met al., 2020,

    Parker solar probe In situ observations of magnetic reconnection exhausts during encounter 1

    , The Astrophysical Journal Supplement, Vol: 246, Pages: 34-34, ISSN: 0067-0049

    Magnetic reconnection in current sheets converts magnetic energy into particle energy. The process may play an important role in the acceleration and heating of the solar wind close to the Sun. Observations from Parker Solar Probe (PSP) provide a new opportunity to study this problem, as it measures the solar wind at unprecedented close distances to the Sun. During the first orbit, PSP encountered a large number of current sheets in the solar wind through perihelion at 35.7 solar radii. We performed a comprehensive survey of these current sheets and found evidence for 21 reconnection exhausts. These exhausts were observed in heliospheric current sheets, coronal mass ejections, and regular solar wind. However, we find that the majority of current sheets encountered around perihelion, where the magnetic field was strongest and plasma β was lowest, were Alfvénic structures associated with bursty radial jets, and these current sheets did not appear to be undergoing local reconnection. We examined conditions around current sheets to address why some current sheets reconnected while others did not. A key difference appears to be the degree of plasma velocity shear across the current sheets: the median velocity shear for the 21 reconnection exhausts was 24% of the Alfvén velocity shear, whereas the median shear across 43 Alfvénic current sheets examined was 71% of the Alfvén velocity shear. This finding could suggest that large, albeit sub-Alfvénic, velocity shears suppress reconnection. An alternative interpretation is that the Alfvénic current sheets are isolated rotational discontinuities that do not undergo local reconnection.
  • Journal article
    Horbury T, Woolley T, Laker R, Matteini L, Eastwood J, Bale SD, Velli M, Chandran BDG, Phan T, Raouafi NE, Goetz K, Harvey PR, Pulupa M, Klein KG, De Wit TD, Kasper JC, Korreck KE, Case AW, Stevens ML, Whittlesey P, Larson D, MacDowall RJ, Malaspina DM, Livi Ret al., 2020,

    Sharp Alfvenic impulses in the near-Sun solar wind

    , The Astrophysical Journal: an international review of astronomy and astronomical physics, Vol: 246, Pages: 1-8, ISSN: 0004-637X

    Measurements of the near-Sun solar wind by Parker Solar Probe have revealed the presence of largenumbers of discrete Alfv ́enic impulses with an anti-Sunward sense of propagation. These are similarto those previously observed near 1 AU, in high speed streams over the Sun’s poles and at 60 solarradii. At 35 solar radii, however, they are typically shorter and sharper than seen elsewhere. Inaddition, these spikes occur in “patches” and there are also clear periods within the same stream whenthey do not occur; the timescale of these patches might be related to the rate at which the spacecraftmagnetic footpoint tracks across the coronal hole from which the plasma originated. While the velocityfluctuations associated with these spikes are typically under 100 km/s, due to the rather low Alfv ́enspeeds in the streams observed by the spacecraft to date, these are still associated with large angulardeflections of the magnetic field - and these deflections are not isotropic. These deflections do notappear to be related to the recently reported large scale, pro-rotation solar wind flow. Estimates ofthe size and shape of the spikes reveal high aspect ratio flow-aligned structures with a transverse scaleof≈104km. These events might be signatures of near-Sun impulsive reconnection events.
  • Journal article
    Martinovic MM, Klein KG, Kasper JC, Case AW, Korreck KE, Larson D, Livi R, Stevens M, Whittlesey P, Chandran BDG, Alterman BL, Huang J, Chen CHK, Bale SD, Pulupa M, Malaspina DM, Bonnell JW, Harvey PR, Goetz K, de Wit TD, MacDowall RJet al., 2020,

    The Enhancement of Proton Stochastic Heating in the Near-Sun Solar Wind

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Tenerani A, Velli M, Matteini L, Reville V, Shi C, Bale SD, Kasper JC, Bonnell JW, Case AW, de Wit TD, Goetz K, Harvey PR, Klein KG, Korreck K, Larson D, Livi R, MacDowall RJ, Malaspina DM, Pulupa M, Stevens M, Whittlesey Pet al., 2020,

    Magnetic field kinks and folds in the solar wind

    , Astrophysical Journal Supplement Series, Vol: 246, Pages: 1-7, ISSN: 0067-0049

    Parker Solar Probe (PSP) observations during its first encounter at 35.7 R ⊙ have shown the presence of magnetic field lines that are strongly perturbed to the point that they produce local inversions of the radial magnetic field, known as switchbacks. Their counterparts in the solar wind velocity field are local enhancements in the radial speed, or jets, displaying (in all components) the velocity–magnetic field correlation typical of large amplitude Alfvén waves propagating away from the Sun. Switchbacks and radial jets have previously been observed over a wide range of heliocentric distances by Helios, Wind, and Ulysses, although they were prevalent in significantly faster streams than seen at PSP. Here we study via numerical magnetohydrodynamics simulations the evolution of such large amplitude Alfvénic fluctuations by including, in agreement with observations, both a radial magnetic field inversion and an initially constant total magnetic pressure. Despite the extremely large excursion of magnetic and velocity fields, switchbacks are seen to persist for up to hundreds of Alfvén crossing times before eventually decaying due to the parametric decay instability. Our results suggest that such switchback/jet configurations might indeed originate in the lower corona and survive out to PSP distances, provided the background solar wind is sufficiently calm, in the sense of not being pervaded by strong density fluctuations or other gradients, such as stream or magnetic field shears, that might destabilize or destroy them over shorter timescales.
  • Journal article
    Szalay JR, Pokorny P, Bale SD, Christian ER, Goetz K, Goodrich K, Hill ME, Kuchner M, Larsen R, Malaspina D, McComas DJ, Mitchell D, Page B, Schwadron Net al., 2020,

    The Near-Sun Dust Environment: Initial Observations fromParker Solar Probe

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Chen CHK, Bale SD, Bonnell JW, Borovikov D, Bowen TA, Burgess D, Case AW, Chandran BDG, de Wit TD, Goetz K, Harvey PR, Kasper JC, Klein KG, Korreck KE, Larson D, Livi R, MacDowall RJ, Malaspina DM, Mallet A, McManus MD, Moncuquet M, Pulupa M, Stevens ML, Whittlesey Pet al., 2020,

    The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Giacalone J, Mitchell DG, Allen RC, Hill ME, McNutt RL, Szalay JR, Desai M, Rouillard AP, Kouloumvakos A, McComas DJ, Christian ER, Schwadron NA, Wiedenbeck ME, Bale S, Brown LE, Case A, Chen X, Cohen CMS, Joyce C, Kasper JC, Klein KG, Korreck K, Larson E, Livi R, Leske RA, MacDowall RJ, Matthaeus WH, Mewaldt RA, Nieves-Chinchilla T, Pulupa M, Roelof EC, Stevens ML, Szabo A, Whittlesey PLet al., 2020,

    Solar Energetic Particles Produced by a Slow Coronal Mass Ejection at similar to 0.25 au

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Leske RA, Christian ER, Cohen CMS, Cummings AC, Davis AJ, Desai M, Giacalone J, Hill ME, Joyce CJ, Krimigis SM, Labrador AW, Malandraki O, Matthaeus WH, McComas DJ, McNutt RL, Mewaldt RA, Mitchell DG, Posner A, Rankin JS, Roelof EC, Schwadron NA, Stone EC, Szalay JR, Wiedenbeck ME, Vourlidas A, Bale SD, MacDowall RJ, Pulupa M, Kasper JC, Allen RC, Case AW, Korreck KE, Livi R, Stevens ML, Whittlesey P, Poduval Bet al., 2020,

    Observations of the 2019 April 4 Solar Energetic Particle Event at theParker Solar Probe

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Stansby D, Matteini L, Horbury TS, Perrone D, D'Amicis R, Bercic Let al., 2020,

    The origin of slow Alfvenic solar wind at solar minimum

    , Monthly Notices of the Royal Astronomical Society, Vol: 492, Pages: 39-44, ISSN: 0035-8711

    Although the origins of slow solar wind are unclear, there is increasing evidence that at least some of it is released in a steady state on overexpanded coronal hole magnetic field lines. This type of slow wind has similar properties to the fast solar wind, including strongly Alfvénic fluctuations. In this study, a combination of proton, alpha particle, and electron measurements are used to investigate the kinetic properties of a single interval of slow Alfvénic wind at 0.35 au. It is shown that this slow Alfvénic interval is characterized by high alpha particle abundances, pronounced alpha–proton differential streaming, strong proton beams, and large alpha-to-proton temperature ratios. These are all features observed consistently in the fast solar wind, adding evidence that at least some Alfvénic slow solar wind also originates in coronal holes. Observed differences between speed, mass flux, and electron temperature between slow Alfvénic and fast winds are explained by differing magnetic field geometry in the lower corona.
  • Journal article
    de Wit TD, Krasnoselskikh VV, Bale SD, Bonnell JW, Bowen TA, Chen CHK, Froment C, Goetz K, Harvey PR, Jagarlamudi VK, Larosa A, MacDowall RJ, Malaspina DM, Matthaeus WH, Pulupa M, Velli M, Whittlesey PLet al., 2020,

    Switchbacks in the Near-Sun Magnetic Field: Long Memory and Impact on the Turbulence Cascade

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Bandyopadhyay R, Goldstein ML, Maruca BA, Matthaeus WH, Parashar TN, Ruffolo D, Chhiber R, Usmanov A, Chasapis A, Qudsi R, Bale SD, Bonnell JW, Dudok de Wit T, Goetz K, Harvey PR, MacDowall RJ, Malaspina DM, Pulupa M, Kasper JC, Korreck KE, Case AW, Stevens M, Whittlesey P, Larson D, Livi R, Klein KG, Velli M, Raouafi Net al., 2020,

    Enhanced Energy Transfer Rate in Solar Wind Turbulence Observed near the Sun from Parker Solar Probe

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Nemecek Z, Durovcova T, Safrankova J, Nemec F, Matteini L, Stansby D, Janitzek N, Berger L, Wimmer-Schweingruber RFet al., 2020,

    What is the solar wind frame of reference?

    , The Astrophysical Journal: an international review of astronomy and astronomical physics, Vol: 889, Pages: 1-14, ISSN: 0004-637X

    Various solar wind ion species move with different speeds and theoretical considerations as well as limited observations in a region close to the Sun show that heavy solar wind ions tend to flow faster than protons, at least in less-aged fast solar wind streams. The solar wind flow carries the frozen-in interplanetary magnetic field (IMF) and this situation evokes three related questions: (i) what is the proper solar wind speed, (ii) is this speed equal to the speed of the dominant component, whatever that may be, and (iii) what is the speed of the magnetic field? We show that simple theoretical considerations based on the MHD approximation as well as on the dynamics of charged particles in electric and magnetic fields suggest that the IMF velocity of motion (de Hoffmann–Teller (HT) velocity) would be deliberated as the velocity appropriate for solar wind studies. Our analysis based on the Wind, Helios, ACE, and SOHO observations of differential streaming of solar wind populations shows that their energy is conserved in the HT frame. On the other hand, the noise and temporal resolution of the data do not allow us to decide whether the total momentum is also conserved in this frame.
  • Journal article
    Huang J, Kasper JC, Vech D, Klein KG, Stevens M, Martinovic MM, Alterman BL, Durovcova T, Paulson K, Maruca BA, Qudsi RA, Case AW, Korreck KE, Jian LK, Velli M, Lavraud B, Hegedus A, Bert CM, Holmes J, Bale SD, Larson DE, Livi R, Whittlesey P, Pulupa M, MacDowall RJ, Malaspina DM, Bonnell JW, Harvey P, Goetz K, de Wit TDet al., 2020,

    Proton Temperature Anisotropy Variations in Inner Heliosphere Estimated with the First <i>Parker Solar Probe</i> Observations

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Chaston CC, Bonnell JW, Bale SD, Kasper JC, Pulupa M, de Wit TD, Bowen TA, Larson DE, Whittlesey PL, Wygant JR, Salem CS, MacDowall RJ, Livi RL, Vech D, Case AW, Stevens ML, Korreck KE, Goetz K, Harvey PR, Malaspina DMet al., 2020,

    MHD Mode Composition in the Inner Heliosphere from the <i>Parker Solar Probe</i>'s First Perihelion

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Wiedenbeck ME, Bucik R, Mason GM, Ho GC, Leske RA, Cohen CMS, Christian ER, Cummings AC, Davis AJ, Desai M, Giacalone J, Haggerty DK, Hill ME, Joyce CJ, Labrador AW, Malandraki O, Matthaeus WH, McComas DJ, McNutt RL, Mewaldt RA, Mitchell DG, Posner A, Rankin JS, Roelof EC, Schwadron NA, Stone EC, Szalay JR, Bale SD, Case AW, Kasper JC, Korreck KE, Larson DE, MacDowall RJ, Pulupa M, Stevens MLet al., 2020,

    <SUP>3</SUP>He-rich Solar Energetic Particle Observations at the <i>Parker Solar Probe</i> and near Earth

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Reville V, Velli M, Panasenco O, Tenerani A, Shi C, Badman ST, Bale SD, Kasper JC, Stevens ML, Korreck KE, Bonnell JW, Case AW, de Wit TD, Goetz K, Harvey PR, Larson DE, Livi R, Malaspina DM, MacDowall RJ, Pulupa M, Whittlesey PLet al., 2020,

    The Role of Alfven Wave Dynamics on the Large-scale Properties of the Solar Wind: Comparing an MHD Simulation with <i>Parker Solar Probe</i> E1 Data

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Page B, Bale SD, Bonnell JW, Goetz K, Goodrich K, Harvey PR, Larsen R, MacDowall RJ, Malaspina DM, Pokorny P, Pulupa M, Szalay JRet al., 2020,

    Examining Dust Directionality with the <i>Parker Solar Probe</i> FIELDS Instrument

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Mozer FS, Agapitov OV, Bale SD, Bonnell JW, Goetz K, Goodrich KA, Gore R, Harvey PR, Kellogg PJ, Malaspina D, Pulupa M, Schumm Get al., 2020,

    Time Domain Structures and Dust in the Solar Vicinity: <i>Parker Solar Probe</i> Observations

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Zhao L-L, Zank GP, Adhikari L, Hu Q, Kasper JC, Bale SD, Korreck KE, Case AW, Stevens M, Bonnell JW, de Wit TD, Goetz K, Harvey PR, MacDowall RJ, Malaspina DM, Pulupa M, Larson DE, Livi R, Whittlesey P, Klein KGet al., 2020,

    Identification of Magnetic Flux Ropes from <i>Parker Solar Probe</i> Observations during the First Encounter

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Qudsi RA, Maruca BA, Matthaeus WH, Parashar TN, Bandyopadhyay R, Chhiber R, Chasapis A, Goldstein ML, Bale SD, Bonnell JW, de Wit TD, Goetz K, Harvey PR, MacDowall RJ, Malaspina D, Pulupa M, Kasper JC, Korreck KE, Case AW, Stevens M, Whittlesey P, Larson D, Livi R, Velli M, Raouafi Net al., 2020,

    Observations of Heating along Intermittent Structures in the Inner Heliosphere from <i>PSP</i> Data

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Rouillard AP, Kouloumvakos A, Vourlidas A, Kasper J, Bale S, Raouafi N-E, Lavraud B, Howard RA, Stenborg G, Stevens M, Poirier N, Davies JA, Hess P, Higginson AK, Lavarra M, Viall NM, Korreck K, Pinto RF, Griton L, Reville V, Louarn P, Wu Y, Dalmasse K, Genot V, Case AW, Whittlesey P, Larson D, Halekas JS, Livi R, Goetz K, Harvey PR, MacDowall RJ, Malaspina D, Pulupa M, Bonnell J, de Witt TD, Penou Eet al., 2020,

    Relating Streamer Flows to Density and Magnetic Structures at the <i>Parker Solar Probe</i>

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Panasenco O, Velli M, D'Amicis R, Shi C, Reville V, Bale SD, Badman ST, Kasper J, Korreck K, Bonnell JW, de Wit TD, Goetz K, Harvey PR, MacDowall RJ, Malaspina DM, Pulupa M, Case AW, Larson D, Livi R, Stevens M, Whittlesey Pet al., 2020,

    Exploring Solar Wind Origins and Connecting Plasma Flows from the <i>Parker Solar Probe</i> to 1 au: Nonspherical Source Surface and Alfvenic Fluctuations

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
  • Journal article
    Chhiber R, Goldstein ML, Maruca BA, Chasapis A, Matthaeus WH, Ruffolo D, Bandyopadhyay R, Parashar TN, Qudsi R, de Wit TD, Bale SD, Bonnell JW, Goetz K, Harvey PR, MacDowall RJ, Malaspina D, Pulupa M, Kasper JC, Korreck KE, Case AW, Stevens M, Whittlesey P, Larson D, Livi R, Velli M, Raouafi Net al., 2020,

    Clustering of Intermittent Magnetic and Flow Structures near <i>Parker</i> <i>Solar Probe</i>'s First Perihelion-A Partial-variance-of-increments Analysis

    , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049

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