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2. Initial results from the New Horizons exploration of 2014 MU69, a small Kuiper Belt Object

Author

Stern, S. A., Weaver, H. A., Spencer, J. R., Olkin, C. B., Gladstone, G. R., Grundy, W. M., Moore, J. M., Cruikshank, D. P., Elliott, H. A., McKinnon, W. B., Parker, J. Wm., Verbiscer, A. J., Young, L. A., Aguilar, D. A., Albers, J. M., Andert, T., Andrews, J. P., Bagenal, F., Banks, M. E., Bauer, B. A., Bauman, J. A., Bechtold, K. E., Beddingfield, C. B., Behrooz, N., Beisser, K. B., Benecchi, S. D., Bernardoni, E., Beyer, R. A., Bhaskaran, S., Bierson, C. J., Binzel, R. P., Birath, E. M., Bird, M. K., Boone, D. R., Bowman, A. F., Bray, V. J., Britt, D. T., Brown, L. E., Buckley, M. R., Buie, M. W., Buratti, B. J., Burke, L. M., Bushman, S. S., Carcich, B., Chaikin, A. L., Chavez, C. L., Cheng, A. F., Colwell, E. J., Conard, S. J., Conner, M. P., Conrad, C. A., Cook, J. C., Cooper, S. B., Custodio, O. S., Ore, C. M. Dalle, Deboy, C. C., Dharmavaram, P., Dhingra, R. D., Dunn, G. F., Earle, A. M., Egan, A. F., Eisig, J., El-Maarry, M. R., Engelbrecht, C., Enke, B. L., Ercol, C. J., Fattig, E. D., Ferrell, C. L., Finley, T. J., Firer, J., Fischetti, J., Folkner, W. M., Fosbury, M. N., Fountain, G. H., Freeze, J. M., Gabasova, L., Glaze, L. S., Green, J. L., Griffith, G. A., Guo, Y., Hahn, M., Hals, D. W., Hamilton, D. P., Hamilton, S. A., Hanley, J. J., Harch, A., Harmon, K. A., Hart, H. M., Hayes, J., Hersman, C. B., Hill, M. E., Hill, T. A., Hofgartner, J. D., Holdridge, M. E., Horányi, M., Hosadurga, A., Howard, A. D., Howett, C. J. A., Jaskulek, S. E., Jennings, D. E., Jensen, J. R., Jones, M. R., Kang, H. K., Katz, D. J., Kaufmann, D. E., Kavelaars, J. J., Keane, J. T., Keleher, G. P., Kinczyk, M., Kochte, M. C., Kollmann, P., Krimigis, S. M., Kruizinga, G. L., Kusnierkiewicz, D. Y., Lahr, M. S., Lauer, T. R., Lawrence, G. B., Lee, J. E., Lessac-Chenen, E. J., Linscott, I. R., Lisse, C. M., Lunsford, A. W., Mages, D. M., Mallder, V. A., Martin, N. P., May, B. H., McComas, D. J., McNutt, R. L., Mehoke, Jr. D. S., Mehoke, T. S., Nelson, D. S., Nguyen, H. D., Núñez, J. I., Ocampo, A. C., Owen, W. M., Oxton, G. K., Parker, A. H., Pätzold, M., Pelgrift, J. Y., Pelletier, F. J., Pineau, J. P., Piquette, M. R., Porter, S. B., Protopapa, S., Quirico, E., Redfern, J. A., Regiec, A. L., Reitsema, H. J., Reuter, D. C., Richardson, D. C., Riedel, J. E., Ritterbush, M. A., Robbins, S. J., Rodgers, D. J., Rogers, G. D., Rose, D. M., Rosendall, P. E., Runyon, K. D., Ryschkewitsch, M. G., Saina, M. M., Salinas, M. J., Schenk, P. M., Scherrer, J. R., Schlei, W. R., Schmitt, B., Schultz, D. J., Schurr, D. C., Scipioni, F., Sepan, R. L., Shelton, R. G., Showalter, M. R., Simon, M., Singer, K. N., Stahlheber, E. W., Stanbridge, D. R., Stansberry, J. A., Steffl, A. J., Strobel, D. F., Stothoff, M. M., Stryk, T., Stuart, J. R., Summers, M. E., Tapley, M. B., Taylor, A., Taylor, H. W., Tedford, R. M., Throop, H. B., Turner, L. S., Umurhan, O. M., Van Eck, J., Velez, D., Versteeg, M. H., Vincent, M. A., Webbert, R. W., Weidner, S. E., Weigle II, G. E., Wendel, J. R., White, O. L., Whittenburg, K. E., Williams, B. G., Williams, K. E., Williams, S. P., Winters, H. L., Zangari, A. M., and Zurbuchen, T. H.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Kuiper Belt is a distant region of the Solar System. On 1 January 2019, the New Horizons spacecraft flew close to (486958) 2014 MU69, a Cold Classical Kuiper Belt Object, a class of objects that have never been heated by the Sun and are therefore well preserved since their formation. Here we describe initial results from these encounter observations. MU69 is a bi-lobed contact binary with a flattened shape, discrete geological units, and noticeable albedo heterogeneity. However, there is little surface color and compositional heterogeneity. No evidence for satellites, ring or dust structures, gas coma, or solar wind interactions was detected. By origin MU69 appears consistent with pebble cloud collapse followed by a low velocity merger of its two lobes., Comment: 43 pages, 8 figure

Published
2020
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3. Plutos interaction with its space environment: Solar Wind, Energetic Particles & Dust

Author

Bagenal, F., Horányi, M., McComas, D. J., McNutt, Jr., R. L., Elliott, H. A., Hill, M. E., Brown, L. E., Delamere, P. A., Kollmann, P., Krimigis, S. M., Kusterer, M., Lisse, C. M., Mitchell, D. G., Piquette, M., Poppe, A. R., Strobel, D. F., Szalay, J. R., Valek, P., Vandegriff, J., Weidner, S., Zirnstein, E. J., Stern, S. A., Ennico, K., Olkin, C. B., Weaver, H. A., and Young, L. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The New Horizons spacecraft carried three instruments that measured the space environment near Pluto as it flew by on 14 July 2015. The Solar Wind Around Pluto instrument revealed an interaction region confined sunward of Pluto to within about 6 Pluto radii. The surprisingly small size is consistent with a reduced atmospheric escape rate as well as a particularly high solar wind flux. The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) observations suggested ions are accelerated and-or deflected around Pluto. In the wake of the interaction region PEPSSI observed suprathermal particle fluxes about one tenth the flux in the interplanetary medium, increasing with distance downstream. The Student Dust Counter, which measures radius greater than 1.4 um grains, detected 1 candidate impact from 5days before to 5 days after closest approach, indicating an upper limit for the dust density in the Pluto system of 4.6 per cubic km.

Published
2016
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4. The Pluto system: Initial results from its exploration by New Horizons

Author

Stern, S. A., Bagenal, F., Ennico, K., Gladstone, G. R., Grundy, W. M., McKinnon, W. B., Moore, J. M., Olkin, C. B., Spencer, J. R., Weaver, H. A., Young, L. A., Andert, T., Andrews, J., Banks, M., Bauer, B., Bauman, J., Barnouin, O. S., Bedini, P., Beisser, K., Beyer, R. A., Bhaskaran, S., Binzel, R. P., Birath, E., Bird, M., Bogan, D. J., Bowman, A., Bray, V. J., Brozovic, M., Bryan, C., Buckley, M. R., Buie, M. W., Buratti, B. J., Bushman, S. S., Calloway, A., Carcich, B., Cheng, A. F., Conard, S., Conrad, C. A., Cook, J. C., Cruikshank, D. P., Custodio, O. S., Ore, C. M. Dalle, Deboy, C., Dischner, Z. J. B., Dumont, P., Earle, A. M., Elliott, H. A., Ercol, J., Ernst, C. M., Finley, T., Flanigan, S. H., Fountain, G., Freeze, M. J., Greathouse, T., Green, J. L., Guo, Y., Hahn, M., Hamilton, D. P., Hamilton, S. A., Hanley, J., Harch, A., Hart, H. M., Hersman, C. B., Hill, A., Hill, M. E., Hinson, D. P., Holdridge, M. E., Horanyi, M., Howard, A. D., Howett, C. J. A., Jackman, C., Jacobson, R. A., Jennings, D. E., Kammer, J. A., Kang, H. K., Kaufmann, D. E., Kollmann, P., Krimigis, S. M., Kusnierkiewicz, D., Lauer, T. R., Lee, J. E., Lindstrom, K. L., Linscott, I. R., Lisse, C. M., Lunsford, A. W., Mallder, V. A., Martin, N., McComas, D. J., McNutt Jr., R. L., Mehoke, D., Mehoke, T., Melin, E. D., Mutchler, M., Nelson, D., Nimmo, F., Nunez, J. I., Ocampo, A., Owen, W. M., Paetzold, M., Page, B., Parker, A. H., Parker, J. W., Pelletier, F., Peterson, J., Pinkine, N., Piquette, M., Porter, S. B., Protopapa, S., Redfern, J., Reitsema, H. J., Reuter, D. C., Roberts, J. H., Robbins, S. J., Rogers, G., Rose, D., Runyon, K., Retherford, K. D., Ryschkewitsch, M. G., Schenk, P., Schindhelm, R., Sepan, B., Showalter, M. R., Singer, K. N., Soluri, M., Stanbridge, D., Steffl, A. J., Strobel, D. F., Stryk, T., Summers, M. E., Szalay, J. R., Tapley, M., Taylor, A., Taylor, H., Throop, H. B., Tsang, C. C. C., Tyler, G. L., Umurhan, O. M., Verbiscer, A. J., Versteeg, M. H., Vincent, M., Webbert, R., Weidner, S., Weigle II, G. E., White, O. L., Whittenburg, K., Williams, B. G., Williams, K., Williams, S., Woods, W. W., Zangari, A. M., and Zirnstein, E.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Pluto system was recently explored by NASA's New Horizons spacecraft, making closest approach on 14 July 2015. Pluto's surface displays diverse landforms, terrain ages, albedos, colors, and composition gradients. Evidence is found for a water-ice crust, geologically young surface units, surface ice convection, wind streaks, volatile transport, and glacial flow. Pluto's atmosphere is highly extended, with trace hydrocarbons, a global haze layer, and a surface pressure near 10 microbars. Pluto's diverse surface geology and long-term activity raise fundamental questions about how small planets remain active many billions of years after formation. Pluto's large moon Charon displays tectonics and evidence for a heterogeneous crustal composition, its north pole displays puzzling dark terrain. Small satellites Hydra and Nix have higher albedos than expected., Comment: 8 pages - Initial Science paper from NASA's New Horizons Pluto Encounter

Published
2015
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7. Pluto's interaction with its space environment: Solar wind, energetic particles, and dust

Author

Bagenal, F., Horányi, M., McComas, D. J., McNutt, R. L., Elliott, H. A., Hill, M. E., Brown, L. E., Delamere, P. A., Kollmann, P., Krimigis, S. M., Kusterer, M., Lisse, C. M., Mitchell, D. G., Piquette, M., Poppe, A. R., Strobel, D. F., Szalay, J. R., Valek, P., Vandegriff, J., Weidner, S., Zirnstein, E. J., Stern, S. A., Ennico, K., Olkin, C. B., Weaver, H. A., and Young, L. A.

Published
2016

8. PLANETARY SCIENCE: Plutoʼs interaction with its space environment: Solar wind, energetic particles, and dust

Author

Bagenal, F., Horányi, M., McComas, D. J., McNutt, R. L., Jr., Elliott, H. A., Hill, M. E., Brown, L. E., Delamere, P. A., Kollmann, P., Krimigis, S. M., Kusterer, M., Lisse, C. M., Mitchell, D. G., Piquette, M., Poppe, A. R., Strobel, D. F., Szalay, J. R., Valek, P., Vandegriff, J., Weidner, S., Zirnstein, E. J., Stern, S. A., Ennico, K., Olkin, C. B., Weaver, H. A., Young, L. A., and Science Team, New Horizons

Published
2016
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9. PLANETARY SCIENCE: The Pluto system: Initial results from its exploration by New Horizons

Author

Stern, S. A., Bagenal, F., Ennico, K., Gladstone, G. R., Grundy, W. M., McKinnon, W. B., Moore, J. M., Olkin, C. B., Spencer, J. R., Weaver, H. A., Young, L. A., Andert, T., Andrews, J., Banks, M., Bauer, B., Bauman, J., Barnouin, O. S., Bedini, P., Beisser, K., Beyer, R. A., Bhaskaran, S., Binzel, R. P., Birath, E., Bird, M., Bogan, D. J., Bowman, A., Bray, V. J., Brozovic, M., Bryan, C., Buckley, M. R., Buie, M. W., Buratti, B. J., Bushman, S. S., Calloway, A., Carcich, B., Cheng, A. F., Conard, S., Conrad, C. A., Cook, J. C., Cruikshank, D. P., Custodio, O. S., Ore, Dalle C. M., Deboy, C., Dischner, Z. J. B., Dumont, P., Earle, A M., Elliott, H. A, Ercol, J., Ernst, C. M., Finley, T., Flanigan, S. H., Fountain, G., Freeze, M. J., Greathouse, T., Green, J. L., Guo, Y., Hahn, M., Hamilton, D. P., Hamilton, S. A., Hanley, J., Harch, A., Hart, H. M., Hersman, C. B., Hill, A., Hill, M. E., Hinson, D. P., Holdridge, M. E., Horanyi, M., Howard, A. D., Howett, C. J. A., Jackman, C., Jacobson, R. A., Jennings, D. E., Kammer, J. A., Kang, H. K., Kaufmann, D. E., Kollmann, P., Krimigis, S. M., Kusnierkiewicz, D., Lauer, T. R., Lee, J. E., Lindstrom, K. L., Linscott, I. R., Lisse, C. M., Lunsford, A. W., Mallder, V. A., Martin, N., McComas, D. J., McNutt, R. L., Jr., Mehoke, D., Mehoke, T., Melin, E. D., Mutchler, M., Nelson, D., Nimmo, F., Nunez, J. I., Ocampo, A., Owen, W. M., Paetzold, M., Page, B., Parker, A. H., Parker, J. W., Pelletier, F., Peterson, J., Pinkine, N., Piquette, M., Porter, S. B., Protopapa, S., Redfern, J., Reitsema, H. J., Reuter, D. C., Roberts, J. H., Bobbins, S. J., Rogers, G., Rose, D., Runyon, K., Retherford, K. D., Ryschkewitsch, M. G., Schenk, P., Schindhelm, E., Sepan, B., Showalter, M. R., Singer, K. N., Soluri, M., Stanbridge, D., Steffl, A. J., Strobel, D. F., Stryk, T., Summers, M. E., Szalay, J. R., Tapley, M., Taylor, A., Taylor, H., Throop, H. B., Tsang, C. C. C., Tyler, G. L., Umurhan, O. M., Verbiscer, A. J., Versteeg, M. H., Vincent, M., Webbert, R., Weidner, S., Weigle, G. E., II, White, O. L., Whittenburg, K., Williams, B. G., Williams, K., Williams, S., Woods, W. W., Zangari, A. M., and Zirnstein, E.

Published
2015
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10. TandEM: Titan and Enceladus mission

Author

Coustenis, A., Atreya, S. K., Balint, T., Brown, R. H., Dougherty, M. K., Ferri, F., Fulchignoni, M., Gautier, D., Gowen, R. A., Griffith, C. A., Gurvits, L. I., Jaumann, R., Langevin, Y., Leese, M. R., Lunine, J. I., McKay, C. P., Moussas, X., Müller-Wodarg, I., Neubauer, F., Owen, T. C., Raulin, F., Sittler, E. C., Sohl, F., Sotin, C., Tobie, G., Tokano, T., Turtle, E. P., Wahlund, J.-E., Waite, J. H., Baines, K. H., Blamont, J., Coates, A. J., Dandouras, I., Krimigis, T., Lellouch, E., Lorenz, R. D., Morse, A., Porco, C. C., Hirtzig, M., Saur, J., Spilker, T., Zarnecki, J. C., Choi, E., Achilleos, N., Amils, R., Annan, P., Atkinson, D. H., Bénilan, Y., Bertucci, C., Bézard, B., Bjoraker, G. L., Blanc, M., Boireau, L., Bouman, J., Cabane, M., Capria, M. T., Chassefière, E., Coll, P., Combes, M., Cooper, J. F., Coradini, A., Crary, F., Cravens, T., Daglis, I. A., de Angelis, E., de Bergh, C., de Pater, I., Dunford, C., Durry, G., Dutuit, O., Fairbrother, D., Flasar, F. M., Fortes, A. D., Frampton, R., Fujimoto, M., Galand, M., Grasset, O., Grott, M., Haltigin, T., Herique, A., Hersant, F., Hussmann, H., Ip, W., Johnson, R., Kallio, E., Kempf, S., Knapmeyer, M., Kofman, W., Koop, R., Kostiuk, T., Krupp, N., Küppers, M., Lammer, H., Lara, L.-M., Lavvas, P., Le Mouélic, S., Lebonnois, S., Ledvina, S., Li, J., Livengood, T. A., Lopes, R. M., Lopez-Moreno, J.-J., Luz, D., Mahaffy, P. R., Mall, U., Martinez-Frias, J., Marty, B., McCord, T., Menor Salvan, C., Milillo, A., Mitchell, D. G., Modolo, R., Mousis, O., Nakamura, M., Neish, C. D., Nixon, C. A., Nna Mvondo, D., Orton, G., Paetzold, M., Pitman, J., Pogrebenko, S., Pollard, W., Prieto-Ballesteros, O., Rannou, P., Reh, K., Richter, L., Robb, F. T., Rodrigo, R., Rodriguez, S., Romani, P., Ruiz Bermejo, M., Sarris, E. T., Schenk, P., Schmitt, B., Schmitz, N., Schulze-Makuch, D., Schwingenschuh, K., Selig, A., Sicardy, B., Soderblom, L., Spilker, L. J., Stam, D., Steele, A., Stephan, K., Strobel, D. F., Szego, K., Szopa, C., Thissen, R., Tomasko, M. G., Toublanc, D., Vali, H., Vardavas, I., Vuitton, V., West, R. A., Yelle, R., and Young, E. F.

Published
2009
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15. Neutral Atmospheres

Author

Mueller-Wodarg, I. C. F., Strobel, D. F., Moses, J. I., Waite, J. H., Crovisier, J., Yelle, R. V., Bougher, S. W., and Roble, R. G.

Published
2008
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16. Mapping the Brightness of Ganymede's Ultraviolet Aurora Using Hubble Space Telescope Observations.

Author

Marzok, A., Schlegel, S., Saur, J., Roth, L., Grodent, D., Strobel, D. F., and Retherford, K. D.

Subjects
SPACE telescopes, GEOMAGNETISM, AURORAS, SOLAR system, PLANETARY atmospheres
Abstract

We analyze Hubble Space Telescope observations of Ganymede made with the Space Telescope Imaging Spectrograph between 1998 and 2017 to generate a brightness map of Ganymede's oxygen emission at 1,356 Å. Our Mercator projected map demonstrates that the brightness along Ganymede's northern and southern auroral ovals strongly varies with longitude. To quantify this variation around Ganymede, we investigate the brightness averaged over 36°‐wide longitude corridors centered around the sub‐Jovian (0° W), leading (90° W), anti‐Jovian (180° W), and trailing (270° W) central longitudes. In the northern hemisphere, the brightness of the auroral oval is 3.7 ± 0.4 times lower in the sub‐Jovian and anti‐Jovian corridors compared to the trailing and leading corridors. The southern oval is overall brighter than the northern oval, and only 2.5 ± 0.2 times fainter on the sub‐ and anti‐Jovian corridors compared to the trailing and leading corridors. This demonstrates that Ganymede's auroral ovals are strongly structured in auroral crescents on the leading side (plasma downstream side) and on the trailing side (plasma upstream side). We also find that the brightness is not symmetric with respect to the 270° meridian, but shifted by ∼20° towards the Jovian‐facing hemisphere. Our map will be useful for subsequent studies to understand the processes that generate the aurora in Ganymede's non‐rotationally driven, sub‐Alfvénic magnetosphere. Plain Language Summary: Northern lights often illuminate the night sky in a shimmering green or red tone at high geographic latitudes. This emission, scientifically referred to as aurora, is a result of electrically charged particles that move along Earth's magnetic field lines and interact with its atmosphere to produce auroral emission. Apart from the Earth, multiple other planets in our solar system also exhibit auroral emission. By characterizing the brightness and structure of these lights, we are therefore able to deduce insights about a planet's atmosphere, magnetic field and the physical processes occurring along the field lines from afar. In this work, we used observations from the Hubble Space Telescope to analyze the auroral emission of Jupiter's largest moon Ganymede. We combined multiple images of Ganymede to create the first complete map that displays the auroral brightness. Our map revealed that the emission on Ganymede's auroral ovals varies strongly in brightness with divisions into two distinct bright and faint regions. They resemble two auroral crescents in the north and south respectively, and demonstrate the uniqueness of Ganymede's aurora in comparison with the auroral ovals of other planets in the solar system. Key Points: Brightness map of Ganymede's ultraviolet auroral emission has been constructed based on Hubble Space Telescope observations from 1998 to 2017Auroral ovals are structured in upstream and downstream "crescents"Brightness on sub‐Jovian and anti‐Jovian side is strongly reduced by a factor of 3–4 compared to upstream and downstream side [ABSTRACT FROM AUTHOR]

Published
2022
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17. The formation of Charons red poles from seasonally cold-trapped volatiles

Author

Grundy, W. M., Cruikshank, D. P., Gladstone, G. R., Howett, C. J. A., Lauer, T. R., Spencer, J. R., Summers, M. E., Buie, M. W., Earle, A. M., Ennico, K., Parker, J. Wm., Porter, S. B., Singer, K. N., Stern, S. A., Verbiscer, A. J., Beyer, R. A., Binzel, R. P., Buratti, B. J., Cook, J. C., Dalle Ore, C. M., Olkin, C. B., Parker, A. H., Protopapa, S., Quirico, E., Retherford, K. D., Robbins, S. J., Schmitt, B., Stansberry, J. A., Umurhan, O. M., Weaver, H. A., Young, L. A., Zangari, A. M., Bray, V. J., Cheng, A. F., McKinnon, W. B., McNutt, R. L., Moore, J. M., Nimmo, F., Reuter, D. C., Schenk, P. M., Bagenal, F., Andert, T., Barnouin, O., Bird, M., Brozovi, M., Elliott, H. A., Greathouse, T. K., Hahn, M., Hamilton, D. P., Hill, M. E., Hinson, D. P., Hofgartner, J., Hornyi, M., Howard, A. D., Jennings, D. E., Kammer, J. A., Kollmann, P., Lavvas, P., Linscott, I. R., Lisse, C. M., Lunsford, A. W., McComas, D. J., McNutt Jr., R. L., Mutchler, M., Nunez, J. I., Paetzold, M., Wm. Parker, J., Philippe, S., Piquette, M., Reitsema, H. J., Roberts, J. H., Runyon, K., Schindhelm, E., Showalter, M. R., Steffl, A. J., Strobel, D. F., Stryk, T., Szalay, J. R., Throop, H. B., Tsang, C. C. C., Tyler, G. L., Versteeg, M. H., Weigle II, G. E., White, O. L., Woods, W. W., and Young, E. F.

Subjects
Charon (Satellite) -- Natural history -- Observations, Pluto (Dwarf planet) -- Natural history -- Observations, Planetary atmospheres -- Natural history -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): W. M. Grundy (corresponding author) [1]; D. P. Cruikshank [2]; G. R. Gladstone [3]; C. J. A. Howett [4]; T. R. Lauer [5]; J. R. Spencer [4]; M. E. [...]

Published
2016
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19. The Dust Halo of Saturn's Largest Icy Moon, Rhea

Author

Jones, G. H., Roussos, E., Krupp, N., Beckmann, U., Coates, A. J., Crary, F., Dandouras, I., Dikarev, V., Dougherty, M. K., Garnier, P., Hansen, C. J., Hendrix, A. R., Hospodarsky, G. B., Johnson, R. E., Kempf, S., Khurana, K. K., Krimigis, S. M., Krüger, H., Kurth, W. S., Lagg, A., McAndrews, H. J., Mitchell, D. G., Paranicas, C., Postberg, F., Russell, C. T., Saur, J., Sei, M., Spahn, F., Srama, R., Strobel, D. F., Tokar, R., Wahlund, J.-E., Wilson, R. J., Woch, J., and Young, D.

Published
2008
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20. Io's Atmospheric Response to Eclipse: UV Aurorae Observations

Author

Retherford, K. D., Spencer, J. R., Stern, S. A., Saur, J., Strobel, D. F., Steffl, A. J., Gladstone, G. R., Weaver, H. A., Cheng, A. F., Parker, J. Wm., Slater, D. C., Versteeg, M. H., Davis, M. W., Bagenal, F., Throop, H. B., Lopes, R. M. C., Reuter, D. C., Lunsford, A., Conard, S. J., Young, L. A., and Moore, J. M.

Published
2007
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21. Titan's Atmospheric Temperatures, Winds, and Composition

Author

Flasar, F. M., Achterberg, R. K., Conrath, B. J., Gierasch, P. J., Kunde, V. G., Nixon, C. A., Bjoraker, G. L., Jennings, D. E., Romani, P. N., Simon-Miller, A. A., Bézard, B., Coustenis, A., Irwin, P. G. J., Teanby, N. A., Brasunas, J., Pearl, J. C., Segura, M. E., Carlson, R. C., Mamoutkine, A., Schinder, P. J., Barucci, A., Courtin, R., Fouchet, T., Gautier, D., Lellouch, E., Marten, A., Prangé, R., Vinatier, S., Strobel, D. F., Calcutt, S. B., Read, P. L., Taylor, F. W., Bowles, N., Samuelson, R. E., Orton, G. S., Spilker, L. J., Owen, T. C., Spencer, J. R., Showalter, M. R., Ferrari, C., Abbas, M. M., Raulin, F., Edgington, S., Ade, P., and Wishnow, E. H.

Published
2005

22. Temperatures, Winds, and Composition in the Saturnian System

Author

Flasar, F. M., Achterberg, R. K., Conrath, B. J., Pearl, J. C., Bjoraker, G. L., Jennings, D. E., Romani, P. N., Simon-Miller, A. A., Kunde, V. G., Nixon, C. A., Bézard, B., Orton, G. S., Spilker, L. J., Spencer, J. R., Irwin, P. G. J., Teanby, N. A., Owen, T. C., Brasunas, J., Segura, M. E., Carlson, R. C., Mamoutkine, A., Gierasch, P. J., Schinder, P. J., Showalter, M. R., Ferrari, C., Barucci, A., Courtin, R., Coustenis, A., Fouchet, T., Gautier, D., Lellouch, E., Marten, A., Prangé, R., Strobel, D. F., Calcutt, S. B., Read, P. L., Taylor, F. W., Bowles, N., Samuelson, R. E., Abbas, M. M., Raulin, F., Ade, P., Edgington, S., Pilorz, S., Wallis, B., and Wishnow, E. H.

Published
2005

23. Jupiter's Atmospheric Composition from the Cassini Thermal Infrared Spectroscopy Experiment

Author

Kunde, V. G., Flasar, F. M., Jennings, D. E., Bézard, B., Strobel, D. F., Conrath, B. J., Nixon, C. A., Bjoraker, G. L., Romani, P. N., Achterberg, R. K., Simon-Miller, A. A., Irwin, P., Brasunas, J. C., Pearl, J. C., Smith, M. D., Orton, G. S., Gierasch, P. J., Spilker, L. J., Carlson, R. C., Mamoutkine, A. A., Calcutt, S. B., Read, P. L., Taylor, F. W., Fouchet, T., Parrish, P., Barucci, A., Courtin, R., Coustenis, A., Gautier, D., Lellouch, E., Marten, A., Prangé, R., Biraud, Y., Ferrari, C., Owen, T. C., Abbas, M. M., Samuelson, R. E., Raulin, F., Ade, P., Césarsky, C. J., Grossman, K. U., and Coradini, A.

Published
2004

29. Constraining the IMF at Pluto Using New Horizons SWAP Data and Hybrid Simulations.

Author

Barnes, N. P., Delamere, P. A., Strobel, D. F., Bagenal, F., McComas, D. J., Elliott, H. A., Valek, P., Weaver, H. A., Ennico, K., Young, L. A., and Stern, S. A.

Subjects
HYBRID computer simulation, SWAPS (Finance), INTERPLANETARY magnetic fields, COSMIC magnetic fields, HEAVY ions
Abstract

New Horizons did not carry a magnetometer, so there is no direct way to know the strength of the Interplanetary Magnetic Field (IMF) at the time of the flyby. Using a hybrid model together with a detailed model of the Solar Wind Around Pluto (SWAP) instrument (McComas et al., 2007, https://doi.org/10.1007/s11214-007-9205-3) we have identified three observables that are sensitive to IMF strength: the width of Pluto's heavy ion tail, the energy of heavy ions, and the profile of thermal pressure along the New Horizons trajectory. By comparing simulation to data we infer that the IMF strength was most likely near or below ∼0.1 nT. We also show that the shell distribution of Interstellar Pickup Ions is important for reproducing these observations due to its effect on global pressure balance. Key Points: Numerical experiments suggest that an IMF strength near or below 0.1 nT is consistent with New Horizons dataHigh plasma beta in the wake adequately explains the broad heavy ion tail that was observedThe shell distribution of interplanetary pickup ions is important for understanding Pluto's plasma wake [ABSTRACT FROM AUTHOR]

Published
2019
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30. The Thermal Structure of Triton's Middle Atmosphere

Author

Elliot, J. L., Strobel, D. F., Zhu, X., Stansberry, J. A., Wasserman, L. H., and Franz, O. G.

Subjects
Triton (Satellite) -- Observations, Atmosphere -- Observations, Astronomy, Earth sciences
Abstract

The atmospheric structure of Triton in the altitude range 25-150 km shows an unexpectedly steep thermal gradient of 0.26 K [km.sup.-1] above 50 km altitude, with a nearly isothermal profile below. The upper part of the profile can be explained by downward conduction of heat deposited by magnetospheric electrons and solar UV. However, the atmospheric temperature below 50 km is too cold for identified radiative processes to dispose of the inferred heat flux (0.0012 erg [cm.sup.-2] [s.sup.-1]) from the upper atmosphere. This implies that either the atmosphere is not in a steady state and/or an unidentified cooling mechanism is at work in the altitude range 25-50 km. When extrapolated to the surface, the inversion results yield a pressure of [MATHEMATICAL EXPRESSION NOT REPRODUCIBLE IN ASCII] [micro]bar, about 5 [micro]bar greater than that observed by Voyager. Key Words: Triton, atmospheres, occultations.

Published
2000

32. Pluto's interaction with the solar wind.

Author

McComas, D. J., Elliott, H. A., Weidner, S., Valek, P., Zirnstein, E. J., Bagenal, F., Delamere, P. A., Ebert, R. W., Funsten, H. O., Horanyi, M., McNutt, R. L., Moser, C., Schwadron, N. A., Strobel, D. F., Young, L. A., Ennico, K., Olkin, C. B., Stern, S. A., and Weaver, H. A.

Published
2016
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50. Far-UV emissions from the SL9 impacts with Jupiter.

Author

Ballester, G. E., Harris, W. M., Gladstone, G. R., Clarke, J. T., Prangé, R., Feldman, P. D., Combi, M. R., Emerich, C., Strobel, D. F., Talavera, A., Budzien, S. A., Vincent, M. B., Livengood, T. A., Jessup, K. L., McGrath, M. A., Hall, D. T., Ajello, J. M., ben Jaffel, L., Rego, D., and Fireman, G.

Published
1995
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