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

Panasenco, O.; Velli, M.; D’Amicis, R.; Shi, Chen; Réville, Victor; Bale, S. D.; Badman, S. T.; Kasper, J. C.; Korreck, K. E.; Bonnell, J. W.; Wit, T. Dudok de; Goetz, K.; Harvey, P.; MacDowall, R. J.; Malaspina, D.; Pulupa, M.; Case, A. W.; Larson, D. E.; Livi, R.; Stevens, Michael L.; Whittlesey, P. L.

doi:10.3847/1538-4365/ab61f4

Cited by 62 publications

(77 citation statements)

References 43 publications

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“…On the other hand, narrow holes expanding above active regions or between pseudostreamers could support a slow wind solution (Panasenco et al 2019). The existence of Alfvènic slow wind, that is, slow wind streams containing the typically fast-wind turbulence made up of outwardly propagating Alfvèn waves (see Panasenco et al 2020 and references therein), may be confirmation of the latter idea.…”

Section: Origin Of Steady and Nonsteady Slow Solar Windmentioning

confidence: 93%

“…In this case, the two spacecraft would actually be traversing the exact same plasma parcel, changed only by ongoing dynamical processes occurring over time τ. Tentative examples of the two types were provided for PSP encounter E1 in Panasenco et al (2020). Again, composition and ionization states should remain unaltered during the transport, meaning that such measurements from SO would allow an essentially unambiguous determination of alignment in this case as well.…”

Section: Synergistic Configurations Of Psp and Somentioning

confidence: 99%

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Understanding the origins of the heliosphere: integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories

Velli

Harra

Vourlidas

et al. 2020

A&A

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Context. The launch of Parker Solar Probe (PSP) in 2018, followed by Solar Orbiter (SO) in February 2020, has opened a new window in the exploration of solar magnetic activity and the origin of the heliosphere. These missions, together with other space observatories dedicated to solar observations, such as the Solar Dynamics Observatory, Hinode, IRIS, STEREO, and SOHO, with complementary in situ observations from WIND and ACE, and ground based multi-wavelength observations including the DKIST observatory that has just seen first light, promise to revolutionize our understanding of the solar atmosphere and of solar activity, from the generation and emergence of the Sun’s magnetic field to the creation of the solar wind and the acceleration of solar energetic particles. Aims. Here we describe the scientific objectives of the PSP and SO missions, and highlight the potential for discovery arising from synergistic observations. Here we put particular emphasis on how the combined remote sensing and in situ observations of SO, that bracket the outer coronal and inner heliospheric observations by PSP, may provide a reconstruction of the solar wind and magnetic field expansion from the Sun out to beyond the orbit of Mercury in the first phases of the mission. In the later, out-of-ecliptic portions of the SO mission, the solar surface magnetic field measurements from SO and the multi-point white-light observations from both PSP and SO will shed light on the dynamic, intermittent solar wind escaping from helmet streamers, pseudo-streamers, and the confined coronal plasma, and on solar energetic particle transport. Methods. Joint measurements during PSP–SO alignments, and magnetic connections along the same flux tube complemented by alignments with Earth, dual PSP–Earth, and SO-Earth, as well as with STEREO-A, SOHO, and BepiColumbo will allow a better understanding of the in situ evolution of solar-wind plasma flows and the full three-dimensional distribution of the solar wind from a purely observational point of view. Spectroscopic observations of the corona, and optical and radio observations, combined with direct in situ observations of the accelerating solar wind will provide a new foundation for understanding the fundamental physical processes leading to the energy transformations from solar photospheric flows and magnetic fields into the hot coronal plasma and magnetic fields and finally into the bulk kinetic energy of the solar wind and solar energetic particles. Results. We discuss the initial PSP observations, which already provide a compelling rationale for new measurement campaigns by SO, along with ground- and space-based assets within the synergistic context described above.

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Section: Origin Of Steady and Nonsteady Slow Solar Windmentioning

confidence: 93%

Section: Synergistic Configurations Of Psp and Somentioning

confidence: 99%

Understanding the origins of the heliosphere: integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories

Velli

Harra

Vourlidas

et al. 2020

A&A

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“…If the latter interpretation is correct, the HCS crossings of future orbits, occurring ever closer to the helmet streamer tips, should shed new light on the instability of the forming HCS and the origin of the slow solar wind. Probe at perihelion appeared to be immersed in solar wind coming from a rapidly expanding small coronal hole Panasenco et al 2020). Though very large magnetic field inversions in the radial magnetic field were observed throughout the interval, these were not reconnecting current sheets but rather large-amplitude Alfvénic structures and rotational discontinuities, associated with bursty radial jets (Kasper et al 2019).…”

Section: Probing Reconnection In Situ: Mms and Parker Solar Probementioning

confidence: 98%

“…2019; Panasenco et al. 2020). Though very large magnetic field inversions in the radial magnetic field were observed throughout the interval, these were not reconnecting current sheets but rather large-amplitude Alfvénic structures and rotational discontinuities, associated with bursty radial jets (Kasper et al.…”

Section: Understanding the Onset Problem: A Common Goal Of Astrophysimentioning

confidence: 99%

Onset of fast magnetic reconnection and particle energization in laboratory and space plasmas

et al. 2020

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The onset of magnetic reconnection in space, astrophysical and laboratory plasmas is reviewed discussing results from theory, numerical simulations and observations. After a brief introduction on magnetic reconnection and approach to the question of onset, we first discuss recent theoretical models and numerical simulations, followed by observations of reconnection and its effects in space and astrophysical plasmas from satellites and ground-based detectors, as well as measurements of reconnection in laboratory plasma experiments. Mechanisms allowing reconnection spanning from collisional resistivity to kinetic effects as well as partial ionization are described, providing a description valid over a wide range of plasma parameters, and therefore applicable in principle to many different astrophysical and laboratory environments. Finally, we summarize the implications of reconnection onset physics for plasma dynamics throughout the Universe and illustrate how capturing the dynamics correctly is important to understanding particle acceleration. The goal of this review is to give a view on the present status of this topic and future interesting investigations, offering a unified approach.

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“…Among different extrapolation methods, the Potential Field Source Surface (PFSS) extrapolation (Hundhausen, 1972) gives an approximate description of the coronal fields from the solar surface to the so-called source surface (a sphere with radius between 1.6 and 3.25 solar radii, with 2.5 often used as standard value (Altschuler and Newkirk, 1969;Hoeksema, 1984)), by assuming the absence of currents in the inner corona (see discussion by Lee et al, 2011). This is a strong assumption (solar eruptions occur only in coronal regions where non-potential field configurations are created), and recent results from Parker Solar Probe are now allowing to measure the non-sphericity of the Source Surface (Panasenco et al, 2020), but the PFSS is often used as a well established technique providing a quite good description of the overall coronal field configuration and the location of open and closed field regions (Nitta et al, 2006;Mandrini et al, 2014). Other extrapolation methods exist, but requires high-resolution vector magnetic fields measurements (De Rosa et al, 2009;Aschwanden, 2016), something that (alike LOS magnetograms) is also not currently available for the whole photosphere.…”

Section: Introductionmentioning

confidence: 99%

Reconstruction of the Parker spiral with the Reverse In situ data and MHD APproach – RIMAP

Biondo

Бемпорад

Mignone

et al. 2021

J. Space Weather Space Clim.

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The reconstruction of plasma parameters in the interplanetary medium is very important to understand the interplanetary propagation of solar eruptions and for Space Weather application purposes. Because only a few spacecraft are measuring in situ these parameters, reconstructions are currently performed by running complex numerical Magneto-hydrodynamic (MHD) simulations starting from remote sensing observations of the Sun. Current models apply full 3D MHD simulations of the corona or extrapolations of photospheric magnetic fields combined with and semiempirical relationships to derive the plasma parameters on a sphere centered on the Sun (inner boundary). The plasma is then propagated in the interplanetary medium up to the Earth’s orbit and beyond. Nevertheless, this approach requires significant theoretical and computational efforts, and the results are only in partial agreement with the in situ observations. In this paper we describe a new approach to this problem called RIMAP - Reverse In situ data and MHD APproach. The plasma parameters in the inner boundary at 0.1 AU are derived directly from the in situ measurements acquired at 1 AU, by applying a back reconstruction technique to remap them into the inner heliosphere. This remapping is done by using the Weber and Davies solar wind theoretical model to reconstruct the wind flowlines. The plasma is then re-propagated outward from 0.1 AU by running a MHD numerical simulation based on the PLUTO code. The interplanetary spiral reconstructions obtained with RIMAP are not only in a much better agreement with the in situ observations, but are also including many more small-scale longitudinal features in the plasma parameters that are not reproduced with the approaches developed so far.

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Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au: Nonspherical Source Surface and Alfvénic Fluctuations

Cited by 62 publications

References 43 publications

Understanding the origins of the heliosphere: integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories

Understanding the origins of the heliosphere: integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories

Onset of fast magnetic reconnection and particle energization in laboratory and space plasmas

Reconstruction of the Parker spiral with the Reverse In situ data and MHD APproach – RIMAP

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