Effect of the two-body currents in the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>H<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mn /><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>n</mml:mi><mml:mo>)</mml:mo><mml:mn /></mml:math>reaction

Lee, Chang-Yong

doi:10.1103/physrevc.55.349

Cited by 2 publications

(3 citation statements)

References 18 publications

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“…Next, we consider the background solar wind solution. Studies have shown that the CME arrival-times modeled by WSA-ENLIL+Cone are sensitive to the accuracy of the background solar wind solution (Lee et al 2013;Mays et al 2015). Temmer et al (2011) compared WSA-ENLIL modeled background solar wind with observations of CME kinematics in interplanetary space and found that the ambient solar wind is able to change the CME kinematics, for example slow CMEs become embedded in the background solar wind.…”

Section: Comparing Ensemble Resultsmentioning

confidence: 99%

“…Ensemble modeling of a CME is a collection of CME arrival-time predictions that represent possible scenarios given the uncertainties associated with initial conditions from observations and modeling (Lee et al 2013;Emmons et al 2013;Mays et al 2015). In addition to giving an average CME arrival-time prediction, this probabilistic forecast allows one to derive an arrival-time uncertainty from the spread and distribution of predictions.…”

Section: Interplanetary Propagationmentioning

confidence: 99%

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Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Mays

Thompson

Jian

et al. 2015

ApJ

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On 7 January 2014 an X1.2 flare and CME with a radial speed ≈ 2500 km s −1 was observed from near an active region close to disk center. This led many forecasters to estimate a rapid arrival at Earth (≈ 36 hours) and predict a strong geomagnetic storm. However, only a glancing CME arrival was observed at Earth with a transit time of ≈ 49 hours and a K P geomagnetic index of only 3−. We study the interplanetary propagation of this CME using the ensemble Wang-Sheeley-Arge (WSA)-ENLIL+Cone model, that allows a sampling of CME parameter uncertainties. We explore a series of simulations to isolate the effects of the background solar wind solution, CME shape, tilt, location, size, and speed, and the results are compared with observed in-situ arrivals at Venus, Earth, and Mars. Our results show that a tilted ellipsoid CME shape improves the initial real-time prediction to better reflect the observed in-situ signatures and the geomagnetic storm strength. CME parameters from the Graduated Cylindrical Shell model used as input to WSA-ENLIL+Cone, along with a tilted ellipsoid cloud shape, improve the arrival-time error by 14.5, 18.7, 23.4 hours for Venus, Earth, and Mars respectively. These results highlight that CME orientation and directionality with respect to observatories play an important role in understanding the propagation of this CME, and for forecasting other glancing CME arrivals. This study also demonstrates the importance of three-dimensional CME fitting made possible by multiple viewpoint imaging. 9 In this coordinate system the Z axis is aligned with the solar north rotation pole and the X axis pointing toward the intersection between the solar equator and the solar central meridian as seen from Earth (Hapgood 1992;Thompson 2006). HEEQ coordinates are related to Stonyhurst heliographic coordinates, with directions south of the origin represented by negative HEEQ latitudes, and directions east by negative HEEQ longitudes.

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Section: Comparing Ensemble Resultsmentioning

confidence: 99%

Section: Interplanetary Propagationmentioning

confidence: 99%

Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Mays

Thompson

Jian

et al. 2015

ApJ

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“…In a recent paper of C.-Y. Lee [49], the author found indeed a large contribution to the 2 H(p, n) inclusive cross section from the exchange of a ρ meson which couples to a "pion-in-flight" in the deuteron. We could not reproduce this result.…”

Section: B Inclusive Spectra Of the 2 H(p N) Reactionmentioning

confidence: 95%

Δ(1232)-nucleon interaction in the2H(p,n)
Mosbacher
¹
,
Osterfeld
²

1997
Phys. Rev. C
16
0
26
3
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The 2 H(p, n) charge exchange reaction at Tp = 790 MeV is used to study the ∆(1232)-nucleon (∆N ) interaction in the ∆ resonance excitation energy region. For the ∆N potential, a meson exchange model is adopted where π, ρ, ω, and σ meson exchanges are taken into account. The deuteron disintegration below and above pion threshold is calculated using a coupled channel approach. Various observables, such as the inclusive cross section, the quasifree ∆ decay, the coherent pion production, and the two-nucleon breakup are considered. It is shown that these observables are influenced by the dynamical treatment of the ∆ degrees of freedom. Of special interest is the coherent pion decay of the ∆ resonance which is studied by means of the exclusive reaction 2 H(p, nπ + ) 2 H. Both the peak energy and the magnitude of the coherent pion production cross section depend very sensitively on the strength of the ∆N potential. The coherent pions have a peak energy of ω = 300 MeV and a strongly forward peaked angular distribution.

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Effect of the two-body currents in the2H(p,n)reaction

Cited by 2 publications

References 18 publications

Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Δ(1232)-nucleon interaction in the2H(p,n)
Mosbacher
¹
,
Osterfeld
²

1997
Phys. Rev. C
16
0
26
3
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Effect of the two-body currents in the2H(p,n)reaction

Cited by 2 publications

References 18 publications

Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Propagation of the 2014 January 7 Cme and Resulting Geomagnetic Non-Event

Δ(1232)-nucleon interaction in the2H(p,n)Mosbacher1, Osterfeld2 1997Phys. Rev. C160263View full textAdd to dashboardCite

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Δ(1232)-nucleon interaction in the2H(p,n)
Mosbacher
¹
,
Osterfeld
²

1997
Phys. Rev. C
16
0
26
3
View full text Add to dashboard Cite