Continuous solar wind forcing knowledge: Providing continuous conditions at Mars with the WSA‐ENLIL + Cone model

Dewey, R. M.; Baker, D. N.; Mays, M. L.; Brain, David; Jakosky, B. M.; Halekas, J. S.; Connerney, J. E. P.; Odstrčil, D.; Luhmann, J. G.; Lee, Christina O.

doi:10.1002/2015ja021941

Cited by 11 publications

(19 citation statements)

References 73 publications

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“…It indicates that the time profile of the estimated upstream solar wind is consistent with that of the typical ICME passage [e.g., Kataoka and Miyoshi , ]. Recently, comparison studies between the undisturbed solar wind observed by MAVEN and the WSA‐ENLIL+Cone model [e.g., Mays et al , ] are well performed by Dewey et al []. We thus also compare these solar wind proxies obtained from the MAVEN observations with the WSA‐ENLIL+Cone model (overplotted as red curves in Figures a–c).…”

Section: Dependence On Upstream Solar Wind Driverssupporting

confidence: 53%

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

et al. 2017

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We present Mars Atmosphere and Volatile EvolutioN (MAVEN) observations of a giant magnetic flux rope in the Martian dayside ionosphere. The flux rope was observed at an altitude of <300 km, downstream from strong subsolar crustal magnetic fields. The peak field amplitude was ∼200 nT, resulting in the largest difference between the observed magnetic field strength and a model for crustal magnetic fields of the entire MAVEN primary science phase. MAVEN detected planetary ions, including H+, O+, and O2+, across the structure. The axial orientation estimated for the flux rope indicates that it likely formed as a result of interactions between the local crustal and overlaid draped interplanetary magnetic fields. Pitch angle distributions of ionospheric photoelectrons imply that this structure is connected to the Martian upper atmosphere. However, the flux rope is not present in observations at the next commensurable orbit crossing (approximately two Martian days later), implying that it eventually detaches from the atmosphere and is carried downstream. The flux rope observations occurred during an interplanetary coronal mass ejection event at Mars, suggesting that the disturbed upstream state played a role in allowing the interplanetary magnetic field to penetrate deeper into the Martian ionosphere than is typical, allowing the formation of the flux rope.

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Section: Dependence On Upstream Solar Wind Driverssupporting

confidence: 53%

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

et al. 2017

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“…From the Earth vantage point, bright CME loops were observed in the southeast quadrant of the LASCO C2 field of view at 04:49 UT and 07:12 UT on 6 March 2015. The two CME merged en route to Mars, based on the LASCO C3 observations and the WSA-Enlil-cone simulations of the two CMEs Dewey et al, 2016]. At Mars, EUVM observed an M2.6 class flare that peaked around 05:50 UT on 6 March.…”

Section: Late February Through March Of 2015mentioning

confidence: 99%

“…Halekas et al, 2016] and/or use model data from WSA-Enlil-cone for estimates of the overall solar wind conditions. For the latter, there is ongoing research activity to improve the modeling accuracy of WSA-Enlil-cone for predicting the upstream conditions at Mars and validate the results with existing upstream solar wind observations [e.g., Falkenberg et al, 2011;Dewey et al, 2016].…”

Section: Periods Of Sep Activity Without Upstream Solar Wind Measuremmentioning

confidence: 99%

MAVEN observations of the solar cycle 24 space weather conditions at Mars

et al. 2017

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The Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft has been continuously observing the variability of solar soft X‐rays and EUV irradiance, monitoring the upstream solar wind and interplanetary magnetic field conditions and measuring the fluxes of solar energetic ions and electrons since its arrival to Mars. In this paper, we provide a comprehensive overview of the space weather events observed during the first ∼1.9 years of the science mission, which includes the description of the solar and heliospheric sources of the space weather activity. To illustrate the variety of upstream conditions observed, we characterize a subset of the event periods by describing the Sun‐to‐Mars details using observations from the MAVEN solar Extreme Ultraviolet Monitor, solar energetic particle (SEP) instrument, Solar Wind Ion Analyzer, and Magnetometer together with solar observations using near‐Earth assets and numerical solar wind simulation results from the Wang‐Sheeley‐Arge‐Enlil model for some global context of the event periods. The subset of events includes an extensive period of intense SEP electron particle fluxes triggered by a series of solar flares and coronal mass ejection (CME) activity in December 2014, the impact by a succession of interplanetary CMEs and their associated SEPs in March 2015, and the passage of a strong corotating interaction region (CIR) and arrival of the CIR shock‐accelerated energetic particles in June 2015. However, in the context of the weaker heliospheric conditions observed throughout solar cycle 24, these events were moderate in comparison to the stronger storms observed previously at Mars.

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“…However, as MAVEN ascends or descends into the BS and other layering regions, there are time periods when there is no method to extract data on solar wind parameters such as the velocity of the plasma, particle density, pressure, temperature, and magnetic field properties. This is where solar wind forecasting models can be utilized to predict supplemental solar wind parameter values (e.g., Dewey et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…To test the model's validity during the two runs, MAVEN's solar wind ion analyzer and magnetometer were used to determine when MAVEN was in upstream solar wind. The SWIA instrument's absolute solar wind density measurements are subject to uncertainties due to ambiguities in the sensitivity calibration as mentioned in Dewey et al (). When comparing MAVEN's proton temperature values to WSA‐ENLIL+Cone estimated temperatures, values derived from SWIA for the orbited averaged data are at times overestimated because temperature is a partial moment of the solar wind plasma distribution.…”

Section: Introductionmentioning

confidence: 99%

Statistical Similarities Between WSA‐ENLIL+Cone Model and MAVEN in Situ Observations From November 2014 to March 2016

et al. 2018

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Normal solar wind flows and intense solar transient events interact directly with the upper Martian atmosphere due to the absence of an intrinsic global planetary magnetic field. Since the launch of the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission, there are now new means to directly observe solar wind parameters at the planet's orbital location for limited time spans. Due to MAVEN's highly elliptical orbit, in situ measurements cannot be taken while MAVEN is inside Mars' magnetosheath. To model solar wind conditions during these atmospheric and magnetospheric passages, this research project utilized the solar wind forecasting capabilities of the WSA‐ENLIL+Cone model. The model was used to simulate solar wind parameters that included magnetic field magnitude, plasma particle density, dynamic pressure, proton temperature, and velocity during a four Carrington rotation‐long segment. An additional simulation that lasted 18 Carrington rotations was then conducted. The precision of each simulation was examined for intervals when MAVEN was in the upstream solar wind, that is, with no exospheric or magnetospheric phenomena altering in situ measurements. It was determined that generalized, extensive simulations have comparable prediction capabilities as shorter, more comprehensive simulations. Generally, this study aimed to quantify the loss of detail in long‐term simulations and to determine if extended simulations can provide accurate, continuous upstream solar wind conditions when there is a lack of in situ measurements.

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Continuous solar wind forcing knowledge: Providing continuous conditions at Mars with the WSA‐ENLIL + Cone model

Cited by 11 publications

References 73 publications

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

MAVEN observations of the solar cycle 24 space weather conditions at Mars

Statistical Similarities Between WSA‐ENLIL+Cone Model and MAVEN in Situ Observations From November 2014 to March 2016

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