C. W. Smith

University of New Hampshire

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R. M. Skoug

Los Alamos National Laboratory

C. Kletzing

University of Iowa

H. E. Spence

University of New Hampshire

J. R. Wygant

University of Minnesota

D. J. McComas

Princeton University

G. D. Reeves

Los Alamos National Laboratory

N. F. Ness

University of Delaware

W. H. Matthaeus

University of Delaware

R. J. MacDowall

Goddard Space Flight Center

W. S. Kŭrth

University of Iowa

Cooperative Institutions

Goddard Space Flight Center

126

University of New Hampshire

116

Charles River Laboratories (Netherlands)

103

University of California, Berkeley

University of Michigan–Ann Arbor

John Wiley & Sons (United States)

Johns Hopkins University Applied Physics Laboratory

Los Alamos National Laboratory

Nagoya University

University of New Hampshire at Manchester

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“Crater” flux transfer events: Highroad to the X line?

Journal of Geophysical Research Atmospheres (2011)

C. J. Farrugia Li‐Jen Chen R. B. Torbert D. J. Southwood S. W. H. Cowley

HAL is

Line (geometry)

10.1029/2010ja015495

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Citations (17)

Quantifying Radiation Belt Electron Precipitation and Its Effect on Atmospheric Chemistry

AGU Fall Meeting Abstracts (2019)

C. Huang H. E. Spence Katharine Duderstadt T. Raeder S. S. Smith

Atmospheric chemistry

Electron precipitation

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Citations (0)

Upstream waves at Uranus

Journal of Geophysical Research Atmospheres (1990)

C. T. Russell R. P. Lepping C. W. Smith

Since the Mach number of the solar wind increases with increasing heliocentric distance, the ratio of thermal to magnetic pressure, or beta, of the Uranian magnetosheath is expected to be much higher than in the terrestrial magnetosheath. Consistent with this expectation the magnetosheath is observed to be extremely turbulent, and we may expect many particles to leak back upstream into the solar wind and/or be scattered from the bow shock. In accord with the expected presence of backstreaming particles, waves of the type associated with terrestrial backstreaming particles are seen outbound along the trajectory of Voyager in the pre‐shock solar wind with frequencies close to 10 −3 Hz. The wave frequency is close to that expected for upstream waves based on measurements closer to the Sun. Upstream from the bow shock the magnetic field was found to be much weaker than expected from observations in the inner solar system. The cause of this depression is unlikely to be the upstream particles; rather the cause is probably intrinsic to the solar wind such as reconnection across the heliospheric current sheet.

Magnetosheath

Uranus

Bow wave

Heliospheric current sheet

10.1029/ja095ia03p02273

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Citations (43)

Interstellar Neutrals, Pickup Ions, and Energetic Neutral Atoms Throughout the Heliosphere: Present Theory and Modeling Overview

Space Science Reviews (2022)

J. M. Sokół H. Kucharek Igor Baliukin H. J. Fahr V. Izmodenov

Abstract Interstellar neutrals (ISNs), pick-up ions (PUIs), and energetic neutral atoms (ENAs) are fundamental constituents of the heliosphere and its interaction with the neighboring interstellar medium. Here, we focus on selected aspects of present-day theory and modeling of these particles. In the last decades, progress in the understanding of the role of PUIs and ENAs for the global heliosphere and its interaction with very local interstellar medium is impressive and still growing. The increasing number of measurements allows for verification and continuing development of the theories and model attempts. We present an overview of various model descriptions of the heliosphere and the processes throughout it including the kinetic, fluid, and hybrid solutions. We also discuss topics in which interplay between theory, models, and interpretation of measurements reveals the complexity of the heliosphere and its understanding. They include model-based interpretation of the ISN, PUI, and ENA measurements conducted from the Earth’s vicinity. In addition, we describe selected processes beyond the Earth’s orbit up to the heliosphere boundary regions, where PUIs significantly contribute to the complex system of the global heliosphere and its interaction with the VLISM.

Heliosphere

Energetic neutral atom

Interplanetary medium

Earth's orbit

10.1007/s11214-022-00883-6

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Citations (17)

Accurate estimation of third-order moments from turbulence measurements

Nonlinear processes in geophysics (2009)

J. J. Podesta M. A. Forman C. W. Smith Daniel C. Elton Y. Malécot

Politano and Pouquet's law, a generalization of Kolmogorov's four-fifths law to incompressible MHD, makes it possible to measure the energy cascade rate in incompressible MHD turbulence by means of third-order moments. In hydrodynamics, accurate measurement of third-order moments requires large amounts of data because the probability distributions of velocity-differences are nearly symmetric and the third-order moments are relatively small. Measurements of the energy cascade rate in solar wind turbulence have recently been performed for the first time, but without careful consideration of the accuracy or statistical uncertainty of the required third-order moments. This paper investigates the statistical convergence of third-order moments as a function of the sample size N. It is shown that the accuracy of the third-moment depends on the number of correlation lengths spanned by the data set and a method of estimating the statistical uncertainty of the third-moment is developed. The technique is illustrated using both wind tunnel data and solar wind data.

Energy cascade

Third order

Central moment

10.5194/npg-16-99-2009

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Citations (27)

The heliospheric magnetic flux, solar wind proton flux, and cosmic ray intensity during the coming solar minimum

Space Weather (2014)

C. W. Smith K. G. McCracken N. A. Schwadron Molly L. Goelzer

Abstract Recent papers have linked the heliospheric magnetic flux to the sunspot cycle with good correlation observed between prediction and observation. Other papers have shown a strong correlation between magnetic flux and solar wind proton flux from coronal holes. We combine these efforts with an expectation that the sunspot activity of the approaching solar minimum will resemble the Dalton or Gleissberg Minimum and predict that the magnetic flux and solar wind proton flux over the coming decade will be lower than at any time during the space age. Using these predictions and established theory, we also predict record high galactic cosmic ray intensities over the same years. The analysis shown here is a prediction of global space climate change within which space weather operates. It predicts a new parameter regime for the transient space weather behavior that can be expected during the coming decade.

Sunspot

Space Weather

Solar cycle 22

Solar minimum

Heliospheric current sheet

Solar maximum

Heliosphere

10.1002/2014sw001067

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Citations (15)

Use of single‐component wind speed in Rankine‐Hugoniot analysis of interplanetary shocks

Space Weather (2011)

Vasiliy S. Vorotnikov C. W. Smith C. J. Farrugia C. J. Meredith Qiang Hu

We have extended and deployed a routine designed to run independently on the Web providing real‐time analysis of interplanetary shock observations from L 1 . The program accesses real‐time magnetic field, solar wind speed, and proton density data from the Advanced Composition Explorer (ACE) spacecraft, searches for interplanetary shocks, analyzes shocks according to the Rankine‐Hugoniot (R‐H) jump conditions, and provides shock solutions on the Web for space weather applications. Because the ACE real‐time data stream contains the wind speed but not the three‐component wind velocity, we describe modifications to the R‐H analysis that use the scalar wind speed and show successful results for analyses of strong interplanetary shocks at 1 AU. We compare the three‐component and one‐component solutions and find the greatest disagreement between the two rests in estimations of the shock speed rather than the shock propagation direction. Uncertainties in magnetic quantities such as magnetic compression and shock normal angle relative to the upstream magnetic field show large uncertainties in both analyses when performed using an automated routine whereas analyses of the shock normal alone do not. The automated data point selection scheme, together with the natural variability of the magnetic field, is inferred to be a problem in a few instances for this and other reasons. For a broad range of interplanetary shocks that arrive 30 to 60 min after passing L 1 , this method will provide 15 to 45 min of advanced warning prior to the shock's collision with the Earth's magnetopause. The shock, in turn, provides advance warning of the approaching driver gas.

10.1029/2010sw000631

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Citations (10)

Forecasting Southward Bz Periods Following Shocks

EGUGA (2018)

Tarik M. Salman Noé Lugaz R. M. Winslow C. J. Farrugia C. W. Smith

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Disentangling the Spatiotemporal Structure of Turbulence Using Multi-Spacecraft Data

Bulletin of the AAS (2023)

Jason TenBarge H. E. Spence James Juno Christopher H. K. Chen C. W. Smith

Whitepaper #387 in the Decadal Survey for Solar and Space Physics (Heliophysics) 2024-2033. Main topics: basic research. Additional topics: fundamental space plasma theory; laboratory space plasma physics.

10.3847/25c2cfeb.9f70da28

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Citations (2)

Technique for measuring and correcting the Taylor microscale

Journal of Geophysical Research Space Physics (2014)

P. Chuychai J. M. Weygand W. H. Matthaeus S. Dasso C. W. Smith

Abstract We discuss and develop methods to estimate and refine measurements of the Taylor microscale from discrete data sets. To study how well a method works, we construct a time series of discrete data with a known power spectrum and Taylor scale, but with various truncations of the resolution that eliminate higher frequencies in a controlled fashion. We compute the second‐order structure function and correlation function, assuming that the unresolved dissipation range spectrum has various values of spectral index. A series of Taylor scale estimates are obtained from parabolic fits to subsets of the correlation function data, and these are extrapolated to the limit of zero separation. The error in this procedure, for finite time resolution sampling, depends on the spectral index in the dissipation range. When the spectral form is known, we can compute a correction factor that improves the estimate of the Taylor microscale value determined from the extrapolation method and band‐limited data. Application of this technique to spacecraft observations of solar wind fluctuations is illustrated.

Microscale chemistry

Taylor microscale

10.1002/2013ja019641

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Citations (9)