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Journal articleMcManus MD, Bowen TA, Mallet A, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 70
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Journal articleDuan D, Bowen TA, Chen CHK, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 40
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Journal articlePulupa M, Bale SD, Badman ST, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 46
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Journal articleMozer FS, Agapitov OV, Bale SD, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 14
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Journal articleZhao L-L, Zank GP, Adhikari L, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 72
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Journal articleQudsi RA, Maruca BA, Matthaeus WH, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 29
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Journal articleRouillard AP, Kouloumvakos A, Vourlidas A, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 60
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Journal articlePanasenco O, Velli M, D'Amicis R, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 55
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Journal articleChhiber R, Goldstein ML, Maruca BA, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 42
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Journal articleSzabo A, Larson D, Whittlesey P, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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Journal articleParashar TN, Goldstein ML, Maruca BA, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 59
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Journal articleMoncuquet M, Meyer-Vernet N, Issautier K, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 147
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Journal articleNieves-Chinchilla T, Szabo A, Korreck KE, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 38
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Journal articleMozer FS, Agapitov OV, Bale SD, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 97
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Journal articleHalekas JS, Whittlesey P, Larson DE, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 125
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Journal articleMitchell DG, Giacalone J, Allen RC, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 21
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Journal articleSchwadron NA, Bale S, Bonnell J, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 26
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Journal articleDesai MI, Mitchell DG, Szalay JR, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 39
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Journal articleCohen CMS, Christian ER, Cummings AC, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 32
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Journal articleChaston CC, Bonnell JW, Bale SD, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 28
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Journal articleHuang J, Kasper JC, Vech D, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 74
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ReportCeppi P, Gregory J, 2020,
Climate sensitivity: What is it, and why is it important?
, Climate sensitivity: What is it, and why is it important?, Publisher: The Grantham Institute, 11Climate sensitivity is a fundamental measure of global climate change. This briefing paper explains how climate sensitivity is estimated from different lines of evidence – modelling, observations, and palaeoclimate records – and why its exact value remains uncertain.
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Journal articleVech D, Kasper JC, Klein KG, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 8
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Journal articleMaksimovic M, Bale SD, Bercic L, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 67
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Journal articlePage B, Bale SD, Bonnell JW, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 32
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Journal articleWiedenbeck ME, Bucik R, Mason GM, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 33
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Journal articleReville V, Velli M, Panasenco O, et al., 2020, , ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 246, ISSN: 0067-0049
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- Citations: 88
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Journal articleEscoubet CP, Hwang K-J, Toledo-Redondo S, et al., 2020, , Frontiers in Astronomy and Space Sciences, Vol: 6, Pages: 1-21, ISSN: 2296-987X
When the supersonic solar wind encounters the Earth's magnetosphere a shock, called bow shock, is formed and the plasma is decelerated and thermalized in the magnetosheath downstream from the shock. Sometimes, however, due to discontinuities in the solar wind, bow shock ripples or ionized dust clouds carried by the solar wind, high speed jets (HSJs) are observed in the magnetosheath. These HSJs have typically a Vx component larger than 200 km s−1 and their dynamic pressure can be a few times the solar wind dynamic pressure. They are typically observed downstream from the quasi-parallel bow shock and have a typical size around one Earth radius (RE) in XGSE. We use a conjunction of Cluster and MMS, crossing simultaneously the magnetopause, to study the characteristics of these HSJs and their impact on the magnetopause. Over 1 h 15 min interval in the magnetosheath, Cluster observed 21 HSJs. During the same period, MMS observed 12 HSJs and entered the magnetosphere several times. A jet was observed simultaneously by both MMS and Cluster and it is very likely that they were two distinct HSJs. This shows that HSJs are not localized into small regions but could span a region larger than 10 RE, especially when the quasi-parallel shock is covering the entire dayside magnetosphere under radial IMF. During this period, two and six magnetopause crossings were observed, respectively, on Cluster and MMS with a significant angle between the observation and the expected normal deduced from models. The angles observed range between from 11° up to 114°. One inbound magnetopause crossing observed by Cluster (magnetopause moving out at 142 km s−1) was observed simultaneous to an outbound magnetopause crossing observed by MMS (magnetopause moving in at −83 km s−1), showing that the magnetopause can have multiple local indentation places, most likely independent from each other. Under the continuous impacts of HSJs, the magnetopause is deformed significan
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Journal articlePerrone D, D'Amicis R, De Marco R, et al., 2020, , Astronomy and Astrophysics: a European journal, Vol: 633, Pages: 1-7, ISSN: 0004-6361
Alfvénic fluctuations in solar wind are an intrinsic property of fast streams, while slow intervals typically have a very low degree of Alfvénicity, with much more variable parameters. However, sometimes a slow wind can be highly Alfvénic. Here we compare three different regimes of solar wind, in terms of Alfvénic content and spectral properties, during a minimum phase of the solar activity and at 0.3 au. We show that fast and Alfvénic slow intervals share some common characteristics. This would suggest a similar solar origin, with the latter coming from over-expanded magnetic field lines, in agreement with observations at 1 au and at the maximum of the solar cycle. Due to the Alfvénic nature of the fluctuations in both fast and Alfvénic slow winds, we observe a well-defined correlation between the flow speed and the angle between magnetic field vector and radial direction. The high level of Alfvénicity is also responsible of intermittent enhancements (i.e. spikes), in plasma speed. Moreover, only for the Alfvénic intervals do we observe a break between the inertial range and large scales, on about the timescale typical of the Alfvénic fluctuations and where the magnetic fluctuations saturate, limited by the magnitude of the local magnetic field. In agreement with this, we recover a characteristic low-frequency 1/f scaling, as expected for fluctuations that are scale-independent. This work is directly relevant for the next solar missions, Parker Solar Probe and Solar Orbiter. One of the goals of these two missions is to study the origin and evolution of slow solar wind. In particular, Parker Solar Probe will give information about the Alfvénic slow wind in the unexplored region much closer to the Sun and Solar Orbiter will allow us to connect the observed physics to the source of the plasma.
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Journal articleShatwell P, Czaja A, Ferreira D, 2020,
<jats:p>To study the role of the Atlantic meridional overturning circulation(AMOC) in climate change, we perform an abrupt CO2-doubling experimentusing a coupled atmosphere-ocean-ice model with a simple geometry thatseparates the ocean into small and large basins. As in observations andhigh-end climate models, the small basin exhibits a MOC and warms at afaster rate than the large basin. In our set-up, this contrast in heatstorage rates is 0.6 +/- 0.1 W/m^2, and we argue that this is due tothe small basin MOC. However, the MOC weakens significantly, yet thishas little impact on the small basin’s heat storage rate. We find thisis due to the effects of both compensating warming patterns andinterbasin heat transports. Thus, although the presence of a MOC isimportant for enhanced heat storage, MOC weakening is surprisinglyunimportant.</jats:p>
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