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1. Interstellar Probe: Humanity's exploration of the Galaxy Begins

Author

Brandt, Pontus C., Provornikova, E.A., Cocoros, A., Turner, D., DeMajistre, R., Runyon, K., Lisse, C.M., Bale, S., Kurth, W.S., Galli, A., Wurz, P., McNutt, Ralph L., Jr., Wimmer-Schweingruber, R., Linsky, J., Redfield, S., Kollmann, P., Mandt, K.E., Rymer, A.M., Roelof, E.C., Kinnison, J., Opher, M., Hill, M.E., and Paul, M.V.

Published
2022
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2. Future Exploration of the Outer Heliosphere and Very Local Interstellar Medium by Interstellar Probe

Author

Brandt, P. C., Provornikova, E., Bale, S. D., Cocoros, A., DeMajistre, R., Dialynas, K., Elliott, H. A., Eriksson, S., Fields, B., Galli, A., Hill, M. E., Horanyi, M., Horbury, T., Hunziker, S., Kollmann, P., Kinnison, J., Fountain, G., Krimigis, S. M., Kurth, W. S., Linsky, J., Lisse, C. M., Mandt, K. E., Magnes, W., McNutt, R. L., Miller, J., Moebius, E., Mostafavi, P., Opher, M., Paxton, L., Plaschke, F., Poppe, A. R., Roelof, E. C., Runyon, K., Redfield, S., Schwadron, N., Sterken, V., Swaczyna, P., Szalay, J., Turner, D., Vannier, H., Wimmer-Schweingruber, R., Wurz, P., and Zirnstein, E. J.

Published
2023
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3. A future interstellar probe on the dynamic heliosphere and its interaction with the very local interstellar medium: In-situ particle and fields measurements and remotely sensed ENAs

Author

Dialynas, K, Sterken, V, Brandt, P, Burlaga, L, Berdichevsky, D, Decker, R, Della Torre, S, Demajistre, R, Galli, A, Gkioulidou, M, Hill, M, Krimigis, S, Kornbleuth, M, Kurth, W, Lavraud, B, Mcnutt, R, Mitchell, D, Mostafavi, P, Nikoukar, R, Opher, M, Provornikova, E, Roelof, E, Rancoita, P, Richardson, J, Roussos, E, Sokol, J, La Vacca, G, Westlake, J, Chen, T, Dialynas K., Sterken V. J., Brandt P. C., Burlaga L., Berdichevsky D. B., Decker R. B., Della Torre S., DeMajistre R., Galli A., Gkioulidou M., Hill M. E., Krimigis S. M., Kornbleuth M., Kurth W., Lavraud B., McNutt R., Mitchell D. G., Mostafavi P. S., Nikoukar R., Opher M., Provornikova E., Roelof E. C., Rancoita P. G., Richardson J. D., Roussos E., Sokol J. M., La Vacca G., Westlake J., Chen T. Y., Dialynas, K, Sterken, V, Brandt, P, Burlaga, L, Berdichevsky, D, Decker, R, Della Torre, S, Demajistre, R, Galli, A, Gkioulidou, M, Hill, M, Krimigis, S, Kornbleuth, M, Kurth, W, Lavraud, B, Mcnutt, R, Mitchell, D, Mostafavi, P, Nikoukar, R, Opher, M, Provornikova, E, Roelof, E, Rancoita, P, Richardson, J, Roussos, E, Sokol, J, La Vacca, G, Westlake, J, Chen, T, Dialynas K., Sterken V. J., Brandt P. C., Burlaga L., Berdichevsky D. B., Decker R. B., Della Torre S., DeMajistre R., Galli A., Gkioulidou M., Hill M. E., Krimigis S. M., Kornbleuth M., Kurth W., Lavraud B., McNutt R., Mitchell D. G., Mostafavi P. S., Nikoukar R., Opher M., Provornikova E., Roelof E. C., Rancoita P. G., Richardson J. D., Roussos E., Sokol J. M., La Vacca G., Westlake J., and Chen T. Y.

Abstract

The recently published Interstellar Probe (ISP) study report describes a pragmatic mission concept with a launch window that starts in 2036 and is expected to reach several hundreds of astronomical units past the heliopause within a time frame of ≥50 years (https://interstellarprobe.jhuapl.edu/Interstellar-Probe-MCR.pdf). Following the ISP report, this paper, that will also be accessible from the Bulletin of the AAS (BAAS) in the framework of the Decadal Survey for Solar and Space Physics (Heliophysics) 2024–2033 (Dialynas et al., A future Interstellar Probe on the dynamic heliosphere and its interaction with the very local interstellar medium: In-situ particle and fields measurements and remotely sensed ENAs, 2022a), aims to highlight the importance of studying the physics of the interactions pertaining to the expanding solar wind that meets the plasma, gas and dust flows of the very local interstellar medium, forming the complex and vast region of our astrosphere. We focus on three fundamental open science questions that reveal the dynamical nature of the heliosphere A) Where are the heliosphere boundaries and how thick is the heliosheath B) Is there a “missing” pressure component towards exploring the dynamics of the global heliosheath and its interaction with the very local interstellar medium C) Why does the shape and size of the global heliosphere appear different in different Energetic Neutral Atom energies? We argue that these questions can only be addressed by exploiting a combination of in-situ charged particle, plasma waves and fields measurements with remotely sensed Energetic Neutral Atoms that can be measured simultaneously from the instruments of a future Interstellar Probe mission, along its trajectory from interplanetary space through the heliosheath and out to the very local interstellar medium.

Published
2023

4. The Interstellar Magnetic Field Close to the Sun II

Author

Frisch, P. C., Andersson, B-G, Berdyugin, A., Piirola, V., DeMajistre, R., Funsten, H. O., Magalhaes, A. M., Seriacopi, D. B., McComas, D. J., Schwadron, N. A., Slavin, J. D., and Wiktorowicz, S. J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

A key indicator of the galactic environment of the Sun is provided by the magnetic field in the interstellar medium (ISM), which influences the shape of the heliosphere. The direction of the nearby interstellar magnetic field (ISMF) is determined from starlight polarized in the ISM. The local ISMF direction is found from the ISMF direction that provides the best fit to the polarization position angles of nearby stars, using weighted fits to the data. New polarization observations are included in the analysis. The best-fitting ISMF is close to the magnetic field direction traced by the center of the Ribbon of energetic neutral atoms, discovered by the Interstellar Boundary Explorer spacecraft. Both the magnetic field and kinematics of the local ISM are consistent with a scenario where the local ISM is a fragment of the Loop I superbubble. An ordered component of the local ISMF is found in a region where PlanetPol data show that polarization increases with distance. It extends to within 8 parsecs of the Sun and implies a weak curvature in the nearby ISMF. Variations from the ordered component indicate turbulence of +/-23 deg. The local ISMF is generally uniform in direction over spatial scales of 8-200 parsecs so that it appears similar to interarm magnetic fields. The best-fitting ISMF direction also agrees with the position of tail-in spatial asymmetries in GeV-TeV galactic cosmic rays. The peculiar geometrical relation between the CMB dipole moment, the heliosphere nose, and local ISMF is supported by these new results. Radiative torques are not likely to play a role in grain alignment for these polarizations., Comment: Accepted by the Astrophysical Journal. Changes from version 1 include addition of an appendix and fixing typos

Published
2012
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5. A future interstellar probe on the dynamic heliosphere and its interaction with the very local interstellar medium: In-situ particle and fields measurements and remotely sensed ENAs

Author

Dialynas K., Sterken V. J., Brandt P. C., Burlaga L., Berdichevsky D. B., Decker R. B., Della Torre S., DeMajistre R., Galli A., Gkioulidou M., Hill M. E., Krimigis S. M., Kornbleuth M., Kurth W., Lavraud B., McNutt R., Mitchell D. G., Mostafavi P. S., Nikoukar R., Opher M., Provornikova E., Roelof E. C., Rancoita P. G., Richardson J. D., Roussos E., Sokol J. M., La Vacca G., Westlake J., Chen T. Y., Dialynas, K, Sterken, V, Brandt, P, Burlaga, L, Berdichevsky, D, Decker, R, Della Torre, S, Demajistre, R, Galli, A, Gkioulidou, M, Hill, M, Krimigis, S, Kornbleuth, M, Kurth, W, Lavraud, B, Mcnutt, R, Mitchell, D, Mostafavi, P, Nikoukar, R, Opher, M, Provornikova, E, Roelof, E, Rancoita, P, Richardson, J, Roussos, E, Sokol, J, La Vacca, G, Westlake, J, and Chen, T

Subjects
Voyager, solar wind, interstellar probe, heliosphere, heliosheath, Cassini, energetic neutral atoms, very local interstellar medium, energetic neutral atom, Astronomy and Astrophysics
Abstract

The recently published Interstellar Probe (ISP) study report describes a pragmatic mission concept with a launch window that starts in 2036 and is expected to reach several hundreds of astronomical units past the heliopause within a time frame of ≥50 years (https://interstellarprobe.jhuapl.edu/Interstellar-Probe-MCR.pdf). Following the ISP report, this paper, that will also be accessible from the Bulletin of the AAS (BAAS) in the framework of the Decadal Survey for Solar and Space Physics (Heliophysics) 2024–2033 (Dialynas et al., A future Interstellar Probe on the dynamic heliosphere and its interaction with the very local interstellar medium: In-situ particle and fields measurements and remotely sensed ENAs, 2022a), aims to highlight the importance of studying the physics of the interactions pertaining to the expanding solar wind that meets the plasma, gas and dust flows of the very local interstellar medium, forming the complex and vast region of our astrosphere. We focus on three fundamental open science questions that reveal the dynamical nature of the heliosphere A) Where are the heliosphere boundaries and how thick is the heliosheath B) Is there a “missing” pressure component towards exploring the dynamics of the global heliosheath and its interaction with the very local interstellar medium C) Why does the shape and size of the global heliosphere appear different in different Energetic Neutral Atom energies? We argue that these questions can only be addressed by exploiting a combination of in-situ charged particle, plasma waves and fields measurements with remotely sensed Energetic Neutral Atoms that can be measured simultaneously from the instruments of a future Interstellar Probe mission, along its trajectory from interplanetary space through the heliosheath and out to the very local interstellar medium., Frontiers in Astronomy and Space Sciences, 10, ISSN:2296-987X

Published
2023

8. Global Observations of the Interstellar Interaction from the Interstellar Boundary Explorer (IBEX)

Author

McComas, D. J., Allegrini, F., Bochsler, P., Bzowski, M., Christian, E. R., Crew, G. B., DeMajistre, R., Fahr, H., Fichtner, H., Frisch, P. C., Funsten, H. O., Fuselier, S. A., Gloeckler, G., Gruntman, M., Heerikhuisen, J., Izmodenov, V., Janzen, P., Knappenberger, P., Krimigis, S., Kucharek, H., Lee, M., Livadiotis, G., Livi, S., MacDowall, R. J., Mitchell, D., Möbius, E., Moore, T., Pogorelov, N. V., Reisenfeld, D., Roelof, E., Saul, L., Schwadron, N. A., Valek, P. W., Vanderspek, R., Wurz, P., and Zank, G. P.

Published
2009
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10. CubeSat Constellation Cloud Winds(C3Winds) A New Wind Observing System to Study Mesoscale Cloud Dynamics and Processes

Author

Wu, D. L, Kelly, M.A, Yee, J.-H, Boldt, J, Demajistre, R, Reynolds, E. L, Tripoli, G. J, Oman, L. D, Prive, N, Heidinger, A. K, and Wanzong, S. T

Subjects
Meteorology And Climatology
Abstract

The CubeSat Constellation Cloud Winds (C3Winds) is a NASA Earth Venture Instrument (EV-I) concept with the primary objective to better understand mesoscale dynamics and their structures in severe weather systems. With potential catastrophic damage and loss of life, strong extratropical and tropical cyclones (ETCs and TCs) have profound three-dimensional impacts on the atmospheric dynamic and thermodynamic structures, producing complex cloud precipitation patterns, strong low-level winds, extensive tropopause folds, and intense stratosphere-troposphere exchange. Employing a compact, stereo IR-visible imaging technique from two formation-flying CubeSats, C3Winds seeks to measure and map high-resolution (2 km) cloud motion vectors (CMVs) and cloud geometric height (CGH) accurately by tracking cloud features within 5-15 min. Complementary to lidar wind observations from space, the high-resolution wind fields from C3Winds will allow detailed investigations on strong low-level wind formation in an occluded ETC development, structural variations of TC inner-core rotation, and impacts of tropopause folding events on tropospheric ozone and air quality. Together with scatterometer ocean surface winds, C3Winds will provide a more comprehensive depiction of atmosphere-boundary-layer dynamics and interactive processes. Built upon mature imaging technologies and long history of stereoscopic remote sensing, C3Winds provides an innovative, cost-effective solution to global wind observations with potential of increased diurnal sampling via CubeSat constellation.

Published
2016

11. The [O.sub.2]([b.sup.1]Σ) dayglow emissions: application to middle and upper atmosphere remote sensing

Author

Yee, Jeng-Hwa, DeMajistre, R., and Morgan, F.

Subjects
Remote sensing -- Research, Auroras -- Research, Atmospheric physics -- Research, Physics
Abstract

The [O.sub.2] atmospheric band transition is observed in the altitude region between ~40 and 200 km in the dayglow and between ~80 and 100 km in the nightglow. Wallace and Hunten (J. Geophys. Res. 73, 4813 (1968)) presented the first detailed analysis of the sources and sinks of this [O.sub.2] airglow emitting state. Because of its extended altitude coverage, bright signal, and spectral and photometric properties, this emission provides an important means to remotely sense the thermal, dynamical, and compositional structures of the upper atmosphere. In this paper we present a photochemical and emission-absorption model that calculates the spectral brightnesses of the four brightest vibrational manifolds of this band system that, for the first time, extends from the mesosphere to the thermosphere. This model incorporates the latest rate constants, cross sections, and spectral parameters relevant to this emission, some of which were not considered in previous remote sensing retrieval applications. The model results are compared with our previous rocket experiments to assess the utility of this emission for upper atmospheric remote sensing and to identify key future measurement challenges. This model, together with improved instrument capabilities, permits us to study the atmosphere from 40 up to 200 km, a region where the strongest coupling between the lower atmosphere and upper atmosphere occurs. PACS Nos.: 07.07.Df, 92.60.hw, 92.60.Vb, 92.60.H Nous observons la bande de transition du [O.sub.2] atmospherique entre les altitudes de ~40 a 200 km dans la lueur diurne et entre ~80 et 100 km dans la lueur nocturne. Wallace et Hunten (J. Geophys. Res. 73, 4813 (1968)) ont presente les premieres analyses sur les sources et les puits d'emission de cette lueur en altitude. A cause du grand domaine en altitude, de la brillance du signal et des proprietes spectrales et photometriques, remission fournit un moyen important pour sonder a distance les structures thermiques, la dynamique et la composition de l'atmosphere superieure. Nous presentons ici un modele de photochimie et d'emission-absorption qui calcule les brillances spectrales des quatre plus brillantes varietes vibrationnelles de ce systeme de bandes qui, pour la premiere fois, s'etend de la mesosphere jusqu'a la thermosphere. Ce modele incorpore les valeurs les plus recentes des constantes de taux, des sections efficaces et des parametres spectraux pertinents au probleme, dont certains n'ont pas ete integres anterieurement dans le processus de sondage a distance. Les resultats du modele sont compares a nos resultats anterieurs obtenus par fusee sonde, afin de valider l'utilisation de cette emission pour le sondage de la haute atmosphere et pour identifier les defis a venir. Ce modele, avec des capacites experimentales ameliorees, nous permet d'etudier l'atmosphere de 40 jusqu'a 200 km d'altitude, une region oh on retrouve le couplage le plus fort entre l'atmosphere basse et l'atmosphere superieure. [Traduit par la Redaction], 1. Introduction The [O.sub.2] atmospheric band emission ([b.sup.1][Σ.sup.+.sub.g]→[X.sup.3][Σ.sup.-.sub.g]) is a bright feature observed in the visible and near infrared region of the airglow spectrum. Since its discovery in the nightglow [...]

Published
2012
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12. The Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) NASA Mission-of-Opportunity

Author

McComas, D. J., Allegrini, F., Baldonado, J., Blake, B., Brandt, P. C., Burch, J., Clemmons, J., Crain, W., Delapp, D., DeMajistre, R., Everett, D., Fahr, H., Friesen, L., Funsten, H., Goldstein, J., Gruntman, M., Harbaugh, R., Harper, R., Henkel, H., Holmlund, C., Lay, G., Mabry, D., Mitchell, D., Nass, U., Pollock, C., Pope, S., Reno, M., Ritzau, S., Roelof, E., Scime, E., Sivjee, M., Skoug, R., Sotirelis, T. S., Thomsen, M., Urdiales, C., Valek, P., Viherkanto, K., Weidner, S., Ylikorpi, T., Young, M., and Zoennchen, J.

Published
2009
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14. Solar Cycle of Imaging the Global Heliosphere: Interstellar Boundary Explorer (IBEX) Observations from 2009–2019

Author

McComas, D. J., primary, Bzowski, M., additional, Dayeh, M. A., additional, DeMajistre, R., additional, Funsten, H. O., additional, Janzen, P. H., additional, Kowalska-Leszczyńska, I., additional, Kubiak, M. A., additional, Schwadron, N. A., additional, Sokół, J. M., additional, Szalay, J. R., additional, Tokumaru, M., additional, and Zirnstein, E. J., additional

Published
2020
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15. Conductance Effects on Inner Magnetospheric Plasma Morphology: Model Comparisons with IMAGE EUV, MENA, and HENA Data

Author

Liemohn, M, Ridley, A. J, Kozyra, J. U, Gallagher, D. L, Brandt, P. C, Henderson, M. G, Denton, M. H, Jahn, J. M, Roelof, E. C, and DeMajistre, R. M

Subjects
Space Radiation
Abstract

Modeling results of the inner magnetosphere showing the influence of the ionospheric conductance on the inner magnetospheric electric fields during the April 17, 2002 magnetic storm are presented. Kinetic plasma transport code results are analyzed in combination with observations of the inner magnetospheric plasma populations, in particular those from the IMAGE satellite. Qualitative and quantitative comparisons are made with the observations from EW, MENA, and HENA, covering the entire energy range simulated by the model (0 to 300 keV). The electric field description, and in particular the ionospheric conductance, is the only variable between the simulations. Results from the data-model comparisons are discussed, detailing the strengths and weaknesses of each conductance choice for each energy channel.

Published
2004

16. A data reduction, management, and analysis system for a 10-terabyte data set

Author

DeMajistre, R and Suther, L

Subjects
Documentation And Information Science
Abstract

Within 12 months a 5-year space-based research investigation with an estimated daily data volume of 10 to 15 gigabytes will be launched. Our instrument/analysis team will analyze 2 to 8 gigabytes per day from this mission. Most of these data will be spatial and multispectral collected from nine sensors covering the UV/Visible/NlR spectrum. The volume and diversity of these data and the nature of its analysis require a very robust reduction and management system. This paper is a summary of the systems requirements and a high-level description of a solution. The paper is intended as a case study of the problems and potential solutions faced by the new generation of Earth observation data support systems.

Published
1995

17. Separation of the Ribbon from Globally Distributed Energetic Neutral Atom Flux Using the First 5 Years of IBEX Observations

Author

Schwadron N. A., Moebius E., Fuselier S. A., McComas D. J., Funsten H. O., Janzen P., Reisenfeld D., Kucharek H., Lee M. A., Fairchild K., Allegrini F., Dayeh M., Livadiotis G., Reno M., Bzowski M., Sokol J. M., Kubiak M. A., Christian E. R., DeMajistre R., Frisch P., Galli A., Wurz P., and Gruntman M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Mathematics::Geometric Topology
Abstract

The Interstellar Boundary Explorer (IBEX) observes the IBEX ribbon which stretches across much of the sky observed in energetic neutral atoms (ENAs). The ribbon covers a narrow (similar to 20 degrees 50 degrees) region that is believed to be roughly perpendicular to the interstellar magnetic field. Superimposed on the IBEX ribbon is the globally distributed flux that is controlled by the processes and properties of the heliosheath. This is a second study that utilizes a previously developed technique to separate ENA emissions in the ribbon from the globally distributed flux. A transparency mask is applied over the ribbon and regions of high emissions. We then solve for the globally distributed flux using an interpolation scheme. Previously ribbon separation techniques were applied to the first year of IBEX Hi data at and above 0.71 keV. Here we extend the separation analysis down to 0.2 keV and to five years of IBEX data enabling first maps of the ribbon and the globally distributed flux across the full sky of ENA emissions. Our analysis shows the broadening of the ribbon peak at energies below 0.71 keV and demonstrates the apparent deformation of the ribbon in the nose and heliotail. We show global asymmetries of the heliosheath including both deflection of the heliotail and differing widths of the lobes in context of the direction draping and compression of the heliospheric magnetic field. We discuss implications of the ribbon maps for the wide array of concepts that attempt to explain the ribbon's origin. Thus we present the five year separation of the IBEX ribbon from the globally distributed flux in preparation for a formal IBEX data release of ribbon and globally distributed flux maps to the heliophysics community.

Published
2014
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19. EFFECTS OF FAST AND SLOW SOLAR WIND ON THE ENERGETIC NEUTRAL ATOM (ENA) SPECTRA MEASURED BY THE INTERSTELLAR BOUNDARY EXPLORER (IBEX) AT THE HELIOSPHERIC POLES

Author

MIT Kavli Institute for Astrophysics and Space Research, Vanderspek, Roland K., Dayeh, M. A., McComas, David J., Allegrini, F., DeMajistre, R., Desai, M. I., Funsten, H. O., Janzen, Paul H., Livadiotis, G., Randol, B. M., Reisenfeld, D. B., Schwadron, N. A., Vanderspek, Roland K, MIT Kavli Institute for Astrophysics and Space Research, Vanderspek, Roland K., Dayeh, M. A., McComas, David J., Allegrini, F., DeMajistre, R., Desai, M. I., Funsten, H. O., Janzen, Paul H., Livadiotis, G., Randol, B. M., Reisenfeld, D. B., Schwadron, N. A., and Vanderspek, Roland K

Abstract

We study the energy dependence of ~0.5-6 keV energetic neutral atom (ENA) spectra in the southern heliospheric polar region obtained during five six-month sky maps measured by IBEX-Hi. We calculate the spectral slopes in the south pole in four different energy bands, namely, ~0.7-1.1 keV, ~1.1-1.7 keV, ~1.7-2.7 keV, and ~2.7-4.3 keV. We show (1) a persistent flattening of the ENA spectrum between ~1 and 2 keV, (2) significantly different modes (2.31, 1.58, 0.97, and 1.44) for the distributions of the slopes in the four different energy bands, and (3) a general decrease with increasing energy in the widths (FWHM) and mode fluctuations (their spread) of the slope distributions. We also compare the averaged ENA spectra measured at the south pole and at mid-latitudes. We conclude that the flattening between ~1 and 2 keV in the polar spectrum (spectral break) is produced by an enhancement of ENAs created by charge exchange between interstellar neutrals and pick-up ions in the fast solar wind., United States. Dept. of Energy, United States. National Aeronautics and Space Administration

Published
2015

20. VARIATIONS IN THE HELIOSPHERIC POLAR ENERGETIC NEUTRAL ATOM FLUX OBSERVED BY THE INTERSTELLAR BOUNDARY EXPLORER

Author

Haystack Observatory, Crew, Geoffrey B., Reisenfeld, D. B., Allegrini, F., Bzowski, M., DeMajistre, R., Frisch, P., Funsten, H. O., Fuselier, S. A., Janzen, Paul H., Kubiak, M. A., Kucharek, Harald, McComas, David J., Roelof, E., Schwadron, N. A., Haystack Observatory, Crew, Geoffrey B., Reisenfeld, D. B., Allegrini, F., Bzowski, M., DeMajistre, R., Frisch, P., Funsten, H. O., Fuselier, S. A., Janzen, Paul H., Kubiak, M. A., Kucharek, Harald, McComas, David J., Roelof, E., and Schwadron, N. A.

Abstract

The ecliptic poles are observed continuously by the Interstellar Boundary Explorer (IBEX); thus, it is possible to discern temporal variations in the energetic neutral atoms (ENAs) from the outer heliosphere on timescales much shorter than the time it takes for IBEX to generate a full sky map (six months). Observations indicate that the ENA flux from the polar directions incident at Earth has been steadily decreasing for the two-year period from 2008 December through 2011 February. Over the IBEX-Hi energy range, the decrease in flux is energy dependent, varying at the south ecliptic pole from no drop at 0.71 keV, to 70% at 1.1 keV. At higher energies the drop ranges between 10% and 50%. The decline observed at the north ecliptic pole is as high as 48%, also at 1.1 keV. The trend correlates with the steady decline in solar wind dynamic pressure observed at 1 AU between 2005 and 2009, the likely period when solar wind protons that provide the source for ENAs observed by IBEX would have been outbound from the Sun. We propose a method by which the correlation between the 1 AU solar wind dynamic pressure and the ENA-derived pressure within the inner heliosheath (IHS) can be used to estimate the distance to the termination shock and the thickness of the IHS in the direction of the ecliptic poles. Our new analysis based on IBEX data shows the TS distances to be 110 AU and 134 AU at the south and north poles, respectively, and the corresponding IHS thicknesses to be 55 AU and 82 AU. Our analysis is consistent with the notion that the observed ENA fluxes originate in the IHS and their variations are driven by the solar wind as it evolves through the solar cycle.

Published
2015

21. SYMMETRY OF THEIBEXRIBBON OF ENHANCED ENERGETIC NEUTRAL ATOM (ENA) FLUX

Author

Funsten, H. O., primary, Bzowski, M., additional, Cai, D. M., additional, Dayeh, M., additional, DeMajistre, R., additional, Frisch, P. C., additional, Heerikhuisen, J., additional, Higdon, D. M., additional, Janzen, P., additional, Larsen, B. A., additional, Livadiotis, G., additional, McComas, D. J., additional, Möbius, E., additional, Reese, C. S., additional, Roelof, E. C., additional, Reisenfeld, D. B., additional, Schwadron, N. A., additional, and Zirnstein, E. J., additional

Published
2015
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22. SPECTRAL EVOLUTION OF ENERGETIC NEUTRAL ATOM EMISSIONS AT THE HELIOSPHERIC POLES AS MEASURED BYIBEXDURING ITS FIRST THREE YEARS

Author

Dayeh, M. A., primary, Allegrini, F., additional, DeMajistre, R., additional, Desai, M. I., additional, Ebert, R. W., additional, Fuselier, S. A., additional, Janzen, P., additional, Livadiotis, G., additional, McComas, D. J., additional, Reisenfeld, D., additional, Schwadron, N. A., additional, and Siewert, M., additional

Published
2014
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23. SEPARATION OF THE RIBBON FROM GLOBALLY DISTRIBUTED ENERGETIC NEUTRAL ATOM FLUX USING THE FIRST FIVE YEARS OF IBEX OBSERVATIONS

Author

Schwadron, N. A., primary, Moebius, E., additional, Fuselier, S. A., additional, McComas, D. J., additional, Funsten, H. O., additional, Janzen, P., additional, Reisenfeld, D., additional, Kucharek, H., additional, Lee, M. A., additional, Fairchild, K., additional, Allegrini, F., additional, Dayeh, M., additional, Livadiotis, G., additional, Reno, M., additional, Bzowski, M., additional, Sokół, J. M., additional, Kubiak, M. A., additional, Christian, E. R., additional, DeMajistre, R., additional, Frisch, P., additional, Galli, A., additional, Wurz, P., additional, and Gruntman, M., additional

Published
2014
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24. IBEX : THE FIRST FIVE YEARS (2009-2013)

Author

McComas, D. J., primary, Allegrini, F., additional, Bzowski, M., additional, Dayeh, M. A., additional, DeMajistre, R., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Gruntman, M., additional, Janzen, P. H., additional, Kubiak, M. A., additional, Kucharek, H., additional, Möbius, E., additional, Reisenfeld, D. B., additional, Schwadron, N. A., additional, Sokół, J. M., additional, and Tokumaru, M., additional

Published
2014
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25. CIRCULARITY OF THEINTERSTELLAR BOUNDARY EXPLORERRIBBON OF ENHANCED ENERGETIC NEUTRAL ATOM (ENA) FLUX

Author

Funsten, H. O., primary, DeMajistre, R., additional, Frisch, P. C., additional, Heerikhuisen, J., additional, Higdon, D. M., additional, Janzen, P., additional, Larsen, B. A., additional, Livadiotis, G., additional, McComas, D. J., additional, Möbius, E., additional, Reese, C. S., additional, Reisenfeld, D. B., additional, Schwadron, N. A., additional, and Zirnstein, E. J., additional

Published
2013
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26. THE INTERSTELLAR MAGNETIC FIELD CLOSE TO THE SUN. II.

Author

Frisch, P. C., primary, Andersson, B-G, additional, Berdyugin, A., additional, Piirola, V., additional, DeMajistre, R., additional, Funsten, H. O., additional, Magalhaes, A. M., additional, Seriacopi, D. B., additional, McComas, D. J., additional, Schwadron, N. A., additional, Slavin, J. D., additional, and Wiktorowicz, S. J., additional

Published
2012
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27. THE FIRST THREE YEARS OF IBEX OBSERVATIONS AND OUR EVOLVING HELIOSPHERE

Author

McComas, D. J., primary, Dayeh, M. A., additional, Allegrini, F., additional, Bzowski, M., additional, DeMajistre, R., additional, Fujiki, K., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Gruntman, M., additional, Janzen, P. H., additional, Kubiak, M. A., additional, Kucharek, H., additional, Livadiotis, G., additional, Möbius, E., additional, Reisenfeld, D. B., additional, Reno, M., additional, Schwadron, N. A., additional, Sokół, J. M., additional, and Tokumaru, M., additional

Published
2012
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28. EXPLORING THE TIME DISPERSION OF THE IBEX -HI ENERGETIC NEUTRAL ATOM SPECTRA AT THE ECLIPTIC POLES

Author

Allegrini, F., primary, Bzowski, M., additional, Dayeh, M. A., additional, DeMajistre, R., additional, Desai, M. I., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Janzen, P. H., additional, Kubiak, M. A., additional, McComas, D. J., additional, Reisenfeld, D. B., additional, Schwadron, N., additional, and Vanderspek, R., additional

Published
2012
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30. VARIATIONS IN THE HELIOSPHERIC POLAR ENERGETIC NEUTRAL ATOM FLUX OBSERVED BY THEINTERSTELLAR BOUNDARY EXPLORER

Author

Reisenfeld, D. B., primary, Allegrini, F., additional, Bzowski, M., additional, Crew, G. B., additional, DeMajistre, R., additional, Frisch, P., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Janzen, P. H., additional, Kubiak, M. A., additional, Kucharek, H., additional, McComas, D. J., additional, Roelof, E., additional, and Schwadron, N. A., additional

Published
2012
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31. SEPARATION OF THEINTERSTELLAR BOUNDARY EXPLORERRIBBON FROM GLOBALLY DISTRIBUTED ENERGETIC NEUTRAL ATOM FLUX

Author

Schwadron, N. A., primary, Allegrini, F., additional, Bzowski, M., additional, Christian, E. R., additional, Crew, G. B., additional, Dayeh, M., additional, DeMajistre, R., additional, Frisch, P., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Goodrich, K., additional, Gruntman, M., additional, Janzen, P., additional, Kucharek, H., additional, Livadiotis, G., additional, McComas, D. J., additional, Moebius, E., additional, Prested, C., additional, Reisenfeld, D., additional, Reno, M., additional, Roelof, E., additional, Siegel, J., additional, and Vanderspek, R., additional

Published
2011
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32. Evolving outer heliosphere: Large‐scale stability and time variations observed by the Interstellar Boundary Explorer

Author

McComas, D. J., primary, Bzowski, M., additional, Frisch, P., additional, Crew, G. B., additional, Dayeh, M. A., additional, DeMajistre, R., additional, Funsten, H. O., additional, Fuselier, S. A., additional, Gruntman, M., additional, Janzen, P., additional, Kubiak, M. A., additional, Livadiotis, G., additional, Möbius, E., additional, Reisenfeld, D. B., additional, and Schwadron, N. A., additional

Published
2010
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39. Partitioning of the reactive nitrogen reservoir in the lower sratosphere of the southern hemisphere: Observations and modeling

Author

Gao, R. S., Gao, R. S., Fahey, D. W., Salawitch, R. J., Lloyd, S. A., Anderson, D. E., DeMajistre, R., McElroy, C. T., Woodbridge, E. L., Wamsley, R. C., Donnelly, S. G., Del Negro, L. A., Proffitt, M. H., Stimpfle, R. M., Kohn, D. W., Kawa, S. R., Lait, L. R., Loewenstein, M., Podolske, J. R., Keim, E. R., Dye, J. E., Wilson, J. C., Chan, K. R., Gao, R. S., Gao, R. S., Fahey, D. W., Salawitch, R. J., Lloyd, S. A., Anderson, D. E., DeMajistre, R., McElroy, C. T., Woodbridge, E. L., Wamsley, R. C., Donnelly, S. G., Del Negro, L. A., Proffitt, M. H., Stimpfle, R. M., Kohn, D. W., Kawa, S. R., Lait, L. R., Loewenstein, M., Podolske, J. R., Keim, E. R., Dye, J. E., Wilson, J. C., and Chan, K. R.

Abstract

Measurements of nitric oxide (NO), nitrogen dioxide (NO2), and total reactive nitrogen (NOy = NO + NO2 + NO3 + HNO3 + ClONO2 + 2N2O5 + ...) were made during austral fall, winter, and spring 1994 as part of the NASA Airborne Southern Hemisphere Ozone Experiment/Measurements for Assessing the Effects of Stratospheric Aircraft mission. Comparisons between measured NO2 values and those calculated using a steady state (SS) approximation are presented for flights at mid and high latitudes. The SS results agree with the measurements to within 8%, suggesting that the kinetic rate coefficients and calculated NO2 photolysis rate used in the SS approximation are reasonably accurate for conditions in the lower stratosphere. However, NO2 values observed in the Concorde exhaust plume were significantly less than SS values. Calculated NO2 photolysis rates showed good agreement with values inferred from solar flux measurements, indicating a strong self-consistency in our understanding of UV radiation transmission in the lower stratosphere. Model comparisons using a full diurnal, photochemical steady state model also show good agreement with the NO and NO2 measurements, suggesting that the reactions affecting the partitioning of the NO2 reservoir are well understood in the lower stratosphere.

Published
1997

44. Nitric oxide abundance in the mesosphere/lower thermosphere region: Roles of solar soft X rays, suprathermal N(4S) atoms, and vertical transport

Author

Swaminathan, P. K., primary, Strobel, D. F., additional, Kupperman, D. G., additional, Kumar, C. Krishna, additional, Acton, L., additional, DeMajistre, R., additional, Yee, J.-H., additional, Paxton, L., additional, Anderson, D. E., additional, Strickland, D. J., additional, and Duff, J. W., additional

Published
1998
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45. Partitioning of the reactive nitrogen reservoir in the lower stratosphere of the southern hemisphere: Observations and modeling

Author

Gao, R. S., primary, Fahey, D. W., additional, Salawitch, R. J., additional, Lloyd, S. A., additional, Anderson, D. E., additional, DeMajistre, R., additional, McElroy, C. T., additional, Woodbridge, E. L., additional, Wamsley, R. C., additional, Donnelly, S. G., additional, Del Negro, L. A., additional, Proffitt, M. H., additional, Stimpfle, R. M., additional, Kohn, D. W., additional, Kawa, S. R., additional, Lait, L. R., additional, Loewenstein, M., additional, Podolske, J. R., additional, Keim, E. R., additional, Dye, J. E., additional, Wilson, J. C., additional, and Chan, K. R., additional

Published
1997
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47. CIRCULARITY OF THE INTERSTELLAR BOUNDARY EXPLORER RIBBON OF ENHANCED ENERGETIC NEUTRAL ATOM (ENA) FLUX.

Author

Funsten, H. O., DeMajistre, R., Frisch, P. C., Heerikhuisen, J., Higdon, D. M., Janzen, P., Larsen, B. A., Livadiotis, G., McComas, D. J., Möbius, E., Reese, C. S., Reisenfeld, D. B., Schwadron, N. A., and Zirnstein, E. J.

Subjects
*ATOMS, *MAGNETIC fields, *KINEMATICS, *HELIOSPHERE, *INTERSTELLAR medium
Abstract

As a sharp feature in the sky, the ribbon of enhanced energetic neutral atom (ENA) flux observed by the Interstellar Boundary Explorer (IBEX) mission is a key signature for understanding the interaction of the heliosphere and the interstellar medium through which we are moving. Over five nominal IBEX energy passbands (0.7, 1.1, 1.7, 2.7, and 4.3 keV), the ribbon is extraordinarily circular, with a peak location centered at ecliptic (λRC, βRC) = (219.°2 ± 1.°3, 39.°9 ± 2.°3) and a half cone angle of ϕC = 74.°5 ± 2.°0. A slight elongation of the ribbon, generally perpendicular to the ribbon center-heliospheric nose vector and with eccentricity ∼0.3, is observed over all energies. At 4.3 keV, the ribbon is slightly larger and displaced relative to lower energies. For all ENA energies, a slice of the ribbon flux peak perpendicular to the circular arc is asymmetric and systematically skewed toward the ribbon center. We derive a spatial coherence parameter δC ⩽ 0.014 that characterizes the spatial uniformity of the ribbon over its extent in the sky and is a key constraint for understanding the underlying processes and structure governing the ribbon ENA emission. [ABSTRACT FROM AUTHOR]

Published
2013
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48. VARIATIONS IN THE HELIOSPHERIC POLAR ENERGETIC NEUTRAL ATOM FLUX OBSERVED BY THE INTERSTELLAR BOUNDARY EXPLORER.

Author

REISENFELD, D. B., ALLEGRINI, F., BZOWSKI, M., CREW, G. B., DEMAJISTRE, R., FRISCH, P., FUNSTEN, H. O., FUSELIER, S. A., JANZEN, P. H., KUBIAK, M. A., KUCHAREK, H., MCCOMAS, D. J., ROELOF, E., and SCHWADRON, N. A.

Subjects
ECLIPTIC, ATOMS, HELIOSPHERE, EARTH (Planet), SOLAR wind, SOLAR cycle
Abstract

The ecliptic poles are observed continuously by the Interstellar Boundary Explorer (IBEX); thus, it is possible to discern temporal variations in the energetic neutral atoms (ENAs) from the outer heliosphere on timescales much shorter than the time it takes for IBEX to generate a full sky map (six months). Observations indicate that the ENA flux from the polar directions incident at Earth has been steadily decreasing for the two-year period from 2008 December through 2011 February. Over the IBEX-Hi energy range, the decrease in flux is energy dependent, varying at the south ecliptic pole from no drop at 0.71 keV, to 70% at 1.1 keV. At higher energies the drop ranges between 10% and 50%. The decline observed at the north ecliptic pole is as high as 48%, also at 1.1 keV. The trend correlates with the steady decline in solar wind dynamic pressure observed at 1 AU between 2005 and 2009, the likely period when solar wind protons that provide the source for ENAs observed by IBEX would have been outbound from the Sun. We propose a method by which the correlation between the 1 AU solar wind dynamic pressure and the ENA-derived pressure within the inner heliosheath (IHS) can be used to estimate the distance to the termination shock and the thickness of the IHS in the direction of the ecliptic poles. Our new analysis based on IBEX data shows the TS distances to be 110 AU and 134 AU at the south and north poles, respectively, and the corresponding IHS thicknesses to be 55 AU and 82 AU. Our analysis is consistent with the notion that the observed ENA fluxes originate in the IHS and their variations are driven by the solar wind as it evolves through the solar cycle. [ABSTRACT FROM AUTHOR]

Published
2012
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50. The Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) NASA Mission-of-Opportunity.

Author

McComas, D., Allegrini, F., Baldonado, J., Blake, B., Brandt, P., Burch, J., Clemmons, J., Crain, W., Delapp, D., DeMajistre, R., Everett, D., Fahr, H., Friesen, L., Funsten, H., Goldstein, J., Gruntman, M., Harbaugh, R., Harper, R., Henkel, H., and Holmlund, C.

Subjects
SPECTROMETER calibration, MAGNETOSPHERE, IMAGING systems in geophysics
Abstract

Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) is a NASA Explorer Mission-of-Opportunity to stereoscopically image the Earth’s magnetosphere for the first time. TWINS extends our understanding of magnetospheric structure and processes by providing simultaneous Energetic Neutral Atom (ENA) imaging from two widely separated locations. TWINS observes ENAs from 1–100 keV with high angular (∼4°×4°) and time (∼1-minute) resolution. The TWINS Ly- α monitor measures the geocoronal hydrogen density to aid in ENA analysis while environmental sensors provide contemporaneous measurements of the local charged particle environments. By imaging ENAs with identical instruments from two widely spaced, high-altitude, high-inclination spacecraft, TWINS enables three-dimensional visualization of the large-scale structures and dynamics within the magnetosphere for the first time. This “instrument paper” documents the TWINS design, construction, calibration, and initial results. Finally, the appendix of this paper describes and documents the Southwest Research Institute (SwRI) instrument calibration facility; this facility was used for all TWINS instrument-level calibrations. [ABSTRACT FROM AUTHOR]

Published
2008
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