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Journal articleMadanian H, Schwartz SJ, Fuselier SA, et al., 2021, , ASTROPHYSICAL JOURNAL LETTERS, Vol: 915, ISSN: 2041-8205
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- Citations: 5
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Journal articleYao Z, Dunn WR, Woodfield EE, et al., 2021, , SCIENCE ADVANCES, Vol: 7, ISSN: 2375-2548
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- Citations: 14
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Journal articleDuan D, He J, Bowen TA, et al., 2021, , Letters of the Astrophysical Journal, Vol: 915, Pages: 1-7, ISSN: 2041-8205
The anisotropy of solar wind turbulence is a critical issue in understanding the physics of energy transfer between scales and energy conversion between fields and particles in the heliosphere. Using the measurement of Parker Solar Probe (PSP), we present an observation of the anisotropy at kinetic scales in the slow, Alfvénic, solar wind in the inner heliosphere. The magnetic compressibility behaves as expected for kinetic Alfvénic turbulence below the ion scale. A steepened transition range is found between the inertial and kinetic ranges in all directions with respect to the local background magnetic field direction. The anisotropy of k⊥ ≫ k∥ is found evident in both transition and kinetic ranges, with the power anisotropy P⊥/P∥ > 10 in the kinetic range leading over that in the transition range and being stronger than that at 1 au. The spectral index varies from αt∥ = −5.7 ± 1.0 to αt⊥ = −3.7 ± 0.3 in the transition range and αk∥ = −3.12 ± 0.22 to αk⊥ = −2.57 ± 0.09 in the kinetic range. The corresponding wavevector anisotropy has the scaling of ${k}_{\parallel }\sim {k}_{\perp }^{0.71\pm 0.17}$ in the transition range, and changes to ${k}_{\parallel }\sim {k}_{\perp }^{0.38\pm 0.09}$ in the kinetic range, consistent with the kinetic Alfvénic turbulence at sub-ion scales.
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Journal articleWang R, Vasko IY, Mozer FS, et al., 2021, , JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, Vol: 126, ISSN: 2169-9380
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- Citations: 29
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Journal articleGristey JJ, Su W, Loeb NG, et al., 2021, , Remote Sensing, Vol: 13, ISSN: 2072-4292
Observing the Earth radiation budget (ERB) from satellites is crucial for monitoring and understanding Earth’s climate. One of the major challenges for ERB observations, particularly for reflected shortwave radiation, is the conversion of the measured radiance to the more energetically relevant quantity of radiative flux, or irradiance. This conversion depends on the solar-viewing geometry and the scene composition associated with each instantaneous observation. We first outline the theoretical basis for algorithms to convert shortwave radiance to irradiance, most commonly known as empirical angular distribution models (ADMs). We then review the progression from early ERB satellite observations that applied relatively simple ADMs, to current ERB satellite observations that apply highly sophisticated ADMs. A notable development is the dramatic increase in the number of scene types, made possible by both the extended observational record and the enhanced scene information now available from collocated imager information. Compared with their predecessors, current shortwave ADMs result in a more consistent average albedo as a function of viewing zenith angle and lead to more accurate instantaneous and mean regional irradiance estimates. One implication of the increased complexity is that the algorithms may not be directly applicable to observations with insufficient accompanying imager information, or for existing or new satellite instruments where detailed scene information is not available. Recent advances that complement and build on the base of current approaches, including machine learning applications and semi-physical calculations, are highlighted.
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Journal articleFarrell WM, Rasca AP, MacDowall RJ, et al., 2021, , ASTROPHYSICAL JOURNAL, Vol: 915, ISSN: 0004-637X
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- Citations: 6
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Journal articleChen L, Ma B, Wu D, et al., 2021, , ASTROPHYSICAL JOURNAL LETTERS, Vol: 915, ISSN: 2041-8205
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- Citations: 7
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Journal articleHalekas JS, Bercic L, Whittlesey P, et al., 2021, , ASTROPHYSICAL JOURNAL, Vol: 916, ISSN: 0004-637X
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- Citations: 22
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Journal articleKuhn- Regnier A, Voulgarakis A, Nowack P, et al., 2021, , Biogeosciences, Vol: 18, Pages: 3861-3879, ISSN: 1726-4170
The seasonal and longer-term dynamics of fuel accumulation affect fire seasonality and the occurrence of extreme wildfires. Failure to account for their influence may help to explain why state-of-the-art fire models do not simulate the length and timing of the fire season or interannual variability in burnt area well. We investigated the impact of accounting for different timescales of fuel production and accumulation on burnt area using a suite of random forest regression models that included the immediate impact of climate, vegetation, and human influences in a given month and tested the impact of various combinations of antecedent conditions in four productivity-related vegetation indices and in antecedent moisture conditions. Analyses were conducted for the period from 2010 to 2015 inclusive. Inclusion of antecedent vegetation conditions representing fuel build-up led to an improvement of the global, climatological out-of-sample R2 from 0.579 to 0.701, but the inclusion of antecedent vegetation conditions on timescales ≥ 1 year had no impact on simulated burnt area. Current moisture levels were the dominant influence on fuel drying. Additionally, antecedent moisture levels were important for fuel build-up. The models also enabled the visualisation of interactions between variables, such as the importance of antecedent productivity coupled with instantaneous drying. The length of the period which needs to be considered varies across biomes; fuel-limited regions are sensitive to antecedent conditions that determine fuel build-up over longer time periods (∼ 4 months), while moisture-limited regions are more sensitive to current conditions that regulate fuel drying.
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Journal articleKuhn-Régnier A, Voulgarakis A, Nowack P, et al., 2021, , Biogeosciences, Vol: 8, ISSN: 1726-4170
The seasonal and longer-term dynamics of fuel accumulation affect fire seasonality and the occurrence of extreme wildfires. Failure to account for their influence mayhelp to explain why state-of-the-art fire models do not simulate the length and timing of the fire season or interannual variability in burnt area well. We investigated the impact of accounting for different timescales of fuel production and accumulation on burnt area using a suite of random forest regression models that included the immediateimpact of climate, vegetation, and human influences in agiven month and tested the impact of various combinationsof antecedent conditions in four productivity-related vegetation indices and in antecedent moisture conditions. Analyses were conducted for the period from 2010 to 2015 inclusive. Inclusion of antecedent vegetation conditions representing fuel build-up led to an improvement of the global,climatological out-of-sample R2from 0.579 to 0.701, but theinclusion of antecedent vegetation conditions on timescales≥ 1 year had no impact on simulated burnt area. Currentmoisture levels were the dominant influence on fuel drying. Additionally, antecedent moisture levels were importantfor fuel build-up. The models also enabled the visualisationof interactions between variables, such as the importanceof antecedent productivity coupled with instantaneous drying. The length of the period which needs to be consideredvaries across biomes; fuel-limited regions are sensitive to antecedent conditions that determine fuel build-up over longertime periods (∼ 4 months), while moisture-limited regionsare more sensitive to current conditions that regulate fuel drying.
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Journal articleMalaspina DM, Wilson LB, Ergun RE, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 13
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Journal articleCohen CMS, Christian ER, Cummings AC, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 19
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Journal articleAkhavan-Tafti M, Kasper J, Huang J, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 20
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Journal articleCattell C, Short B, Breneman A, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 24
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Journal articleFinley AJ, McManus MD, Matt SP, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 12
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Journal articleHarra L, Brooks DH, Bale SD, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 20
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Journal articleSchwadron NA, Joyce CJ, Aly A, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 12
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Journal articlePhan TD, Lavraud B S J, Halekas, et al., 2021, , Astronomy & Astrophysics, Vol: 650, Pages: 1-14, ISSN: 0004-6361
During three of its first five orbits around the Sun, Parker Solar Probe (PSP) crossed the large-scale Heliospheric Current Sheet (HCS)multiple times and provided unprecedented detailed plasma and field observations of the near-Sun HCS. We report the commondetections by PSP of reconnection exhaust signatures in the HCS at heliocentric distances of 29.5-107 solar radii during Encounters1, 4 and 5. Both sunward and antisunward-directed reconnection exhausts were observed. In the sunward reconnection exhausts,PSP detected counterstreaming strahl electrons, indicating that HCS reconnection resulted in the formation of closed magnetic fieldlines with both ends connected to the Sun. In the antisunward exhausts, PSP observed dropouts of strahl electrons, consistent withthe reconnected HCS field lines being disconnected from the Sun. The common detection of reconnection in the HCS suggests thatreconnection is almost always active in the HCS near the Sun. Furthermore, the occurrence of multiple long-duration partial crossingsof the HCS suggests that HCS reconnection could produce chains of large bulges with spatial dimensions of up to several solarradii. The finding of the prevalence of reconnection in the HCS is somewhat surprising since PSP has revealed that the HCS is muchthicker than the kinetic scales required for reconnection onset. The observations are also in stark contrast with the apparent absenceof reconnection in most of the small-scale and much more intense current sheets encountered near perihelia, many of which areassociated with ‘switchbacks’. Thus, the PSP findings suggest that large-scale dynamics either locally in the solar wind or within thecoronal source of the HCS (at the tip of helmet streamers) plays a critical role in triggering reconnection onset.
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Journal articleFargette N, Lavraud B, Rouillard A, et al., 2021, , Astronomy & Astrophysics, Vol: 650, Pages: 1-12, ISSN: 0004-6361
Aims. We report the observation by Parker Solar Probe (PSP) of magnetic structures in the solar wind that present a strong peak intheir magnetic field magnitude with an embedded central current sheet. Similar structures have been observed, either at the Earth’smagnetopause and called interlinked flux tubes, or in the solar wind and called interplanetary field enhancements.Methods. In this work, we first investigate two striking events in detail; one occurred in the regular slow solar wind on November 2,2018 and the other was observed during a heliospheric current sheet crossing on November 13, 2018. They both show the presenceof a central current sheet with a visible ion jet and general characteristics consistent with the occurrence of magnetic reconnection.We then performed a survey of PSP data from encounters 1 to 4 and find 18 additional events presenting an increase in the magneticfield magnitude of over 30% and a central current sheet. We performed a statistical study on the 20 "magnetic increases with centralcurrent sheet" (MICCS), with 13 observed in the regular slow solar wind with a constant polarity (i.e., identical strahl direction), and7 which were specifically observed near a heliospheric current sheet (HCS) crossing.Results. We analyze and discuss the general properties of the structures, including the duration, location, amplitude, and magnetictopology, as well as the characteristics of their central current sheet. We find that the latter has a preferential orientation in the TNplane of the RTN frame. We also find no significant change in the dust impact rate in the vicinity of the MICCS under study, leadingus to conclude that dust probably plays no role in the MICCS formation and evolution. Our findings are overall consistent with adouble flux tube-configuration that would result from initially distinct flux tubes which interact during solar wind propagation.
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Journal articleChen CHK, Chandran BDG, Woodham LD, et al., 2021, , Astronomy & Astrophysics, Vol: 650, Pages: 1-6, ISSN: 0004-6361
The fourth orbit of Parker Solar Probe (PSP) reached heliocentric distances down to 27.9 R⊙, allowing solar wind turbulence and acceleration mechanisms to be studied in situ closer to the Sun than previously possible. The turbulence properties were found to be significantly different in the inbound and outbound portions of PSP’s fourth solar encounter, which was likely due to the proximity to the heliospheric current sheet (HCS) in the outbound period. Near the HCS, in the streamer belt wind, the turbulence was found to have lower amplitudes, higher magnetic compressibility, a steeper magnetic field spectrum (with a spectral index close to –5/3 rather than –3/2), a lower Alfvénicity, and a ‘1∕f’ break at much lower frequencies. These are also features of slow wind at 1 au, suggesting the near-Sun streamer belt wind to be the prototypical slow solar wind. The transition in properties occurs at a predicted angular distance of ≈4° from the HCS, suggesting ≈8° as the full-width of the streamer belt wind at these distances. While the majority of the Alfvénic turbulence energy fluxes measured by PSP are consistent with those required for reflection-driven turbulence models of solar wind acceleration, the fluxes in the streamer belt are significantly lower than the model predictions, suggesting that additional mechanisms are necessary to explain the acceleration of the streamer belt solar wind.
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Journal articleLiu M, Issautier K, Meyer-Vernet N, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 21
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Journal articleZhao L-L, Zank GP, Hu Q, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 49
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Journal articleLarosa A, Krasnoselskikh V, de Wit TD, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 51
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Journal articleBadman ST, Bale SD, Rouillard AP, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 29
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Journal articleBandyopadhyay R, Matthaeus WH, McComas DJ, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 16
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Journal articleJoyce CJ, McComas DJ, Schwadron NA, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 16
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Journal articleFroment C, Krasnoselskikh V, de Wit TD, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 36
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Journal articleJagarlamudi VK, de Wit TD, Froment C, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 30
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Journal articleShi C, Velli M, Panasenco O, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 42
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Journal articleHalekas JS, Whittlesey PL, Larson DE, et al., 2021, , ASTRONOMY & ASTROPHYSICS, Vol: 650, ISSN: 0004-6361
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- Citations: 32
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