Shocks in the Very Local Interstellar Medium by Mostafavi, P., Burlaga, L. F., Cairns, I. H., Fuselier, S. A., Fraternale, F., Gurnett, D. A., Kim, T. K., Kurth, W. S., Pogorelov, N. V., Provornikova, E., Richardson, J. D., Turner, D. L., Zank, G. P.

“…Abstract Large-scale disturbances generated by the Sun’s dynamics first propagate through the heliosphere, influence the heliosphere’s outer boundaries, and then traverse and modify the very local interstellar medium (VLISM). The existence of shocks in the VLISM was initially suggested by Voyager observations of the 2-3 kHz radio emissions in the heliosphere. …”
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Observations of the Outer Heliosphere, Heliosheath, and Interstellar Medium by Richardson, J. D., Burlaga, L. F., Elliott, H., Kurth, W. S., Liu, Y. D., von Steiger, R.

“…Abstract The Voyager spacecraft have left the heliosphere and entered the interstellar medium, making the first observations of the termination shock, heliosheath, and heliopause. …”
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Voyager observations of the interaction of the heliosphere with the interstellar medium by Richardson, John D.

“…This paper provides a brief review and update on the Voyager observations of the interaction of the heliosphere with the interstellar medium. Voyager has found many surprises: (1) a new energetic particle component which is accelerated at the termination shock (TS) and leaks into the outer heliosphere forming a foreshock region; (2) a termination shock which is modulated by energetic particles and which transfers most of the solar wind flow energy to the pickup ions (not the thermal ions); (3) the heliosphere is asymmetric; (4) the TS does not accelerate anomalous cosmic rays at the Voyager locations; and (5) the plasma flow in the Voyagers 1 (V1) and 2 (V2) directions are very different. …”
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Simulating the interstellar medium of galaxies with radiative transfer, non-equilibrium thermochemistry, and dust by Kannan, Rahul, Marinacci, Federico, Vogelsberger, Mark, Sales, Laura V, Torrey, Paul, Springel, Volker, Hernquist, Lars

“…We present a novel framework to self-consistently model the effects of radiation fields, dust physics, and molecular chemistry (H2) in the interstellar medium (ISM) of galaxies. The model combines a state-of-the-art radiation hydrodynamics module with a H  and He  non-equilibrium thermochemistry module that accounts for H2 coupled to an empirical dust formation and destruction model, all integrated into the new stellar feedback framework SMUGGLE. …”
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Simulating the interstellar medium and stellar feedback on a moving mesh: implementation and isolated galaxies by Marinacci, Federico, Sales, Laura V, Vogelsberger, Mark, Torrey, Paul, Springel, Volker

“…This novel sub-resolution model resolves the multiphase gas structure of the interstellar medium and selfconsistently generates gaseous outflows. …”
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The Early History of Heliospheric Science and the Spacecraft That Made It Possible by Zank, G. P., Sterken, V., Giacalone, J., Möbius, E., von Steiger, R., Stone, E. S., Krimigis, S. M., Richardson, J. D., Linsky, J., Izmodenov, V., Heber, B.

“…Abstract Our understanding of the interaction of the large-scale heliosphere with the local interstellar medium (LISM) has undergone a profound change since the very earliest analyses of the problem. …”
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Interstellar Mapping and Acceleration Probe (IMAP): A New NASA Mission by McComas, D. J, Christian, E. R, Schwadron, N. A, Fox, N., Westlake, J., Allegrini, F., Baker, D. N, Biesecker, D., Bzowski, M., Clark, G., Cohen, C. M S, Cohen, I., Dayeh, M. A, Decker, R., de Nolfo, G. A, Desai, M. I, Ebert, R. W, Elliott, H. A, Fahr, H., Frisch, P. C, Funsten, H. O, Fuselier, S. A, Galli, A., Galvin, A. B, Giacalone, J., Gkioulidou, M., Guo, F., Horanyi, M., Isenberg, P., Janzen, P., Kistler, L. M, Korreck, K., Kubiak, M. A, Kucharek, H., Larsen, B. A, Leske, R. A, Lugaz, N., Luhmann, J., Matthaeus, W., Mitchell, D., Moebius, E., Ogasawara, K., Reisenfeld, D. B, Russell, C. T, Sokół, J. M, Spence, H. E, Skoug, R., Sternovsky, Z., Swaczyna, P., Szalay, J. R, Tokumaru, M., Wiedenbeck, M. E, Wurz, P., Zank, G. P, Zirnstein, E. J, Richardson, John D.

“…Keywords: Heliosphere, Interstellar medium, IBEX, IMAP, ENA, Energetic particle…”
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PRESSURE PULSES AT by Wang, C., Liu, Y. D., Šafránková, J., Němeček, Z., Kurth, W. S., Richardson, John D.

“…Voyager 1 (V1) crossed the heliopause into the local interstellar medium (LISM) in 2012. The LISM is a dynamic region periodically disturbed by solar transients with outward-propagating shocks, cosmic-ray intensity changes and anisotropies, and plasma wave oscillations. …”
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PLASMA NEAR THE HELIOSHEATH: OBSERVATIONS AND MODELING by Borovikov, Sergey N., Pogorelov, Nikolai V., Burlaga, L. F., Richardson, John D.

“…Sound numerical modeling is capable of providing important predictive information about the solar wind interaction with the local interstellar medium. The results of our three-dimensional simulation show a good agreement with Voyager observations from 2007 to 2010. …”
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VOYAGER OBSERVATIONS OF MAGNETIC SECTORS AND HELIOSPHERIC CURRENT SHEET CROSSINGS IN THE OUTER HELIOSPHERE by Burlaga, L. F., Drake, J. F., Hill, M. E., Opher, M., Richardson, John D.

“…Voyager 1 (V1) has passed through the heliosheath and is in the local interstellar medium. Voyager 2 (V2) has been in the heliosheath since 2007. …”
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Observations of fast radio bursts at frequencies down to 400 megahertz by The CHIME/FRB Collaboration, Masui, Kiyoshi, Mena Parra, Juan David

“…The overall scattering properties of our sample suggest that FRBs as a class are preferentially located in environments that scatter radio waves more strongly than in the diffuse interstellar medium in the Milky Way.…”
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Modeling Fast Radio Burst Dispersion and Scattering Properties in the First CHIME/FRB Catalog by Masui, Kiyoshi

“…Our simulations confirm the results of previous population studies, which suggested that the interstellar medium of the host galaxy alone (simulated based on the NE2001 model) cannot explain the observed scattering timescales of FRBs. …”
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The Solar Wind in the Outer Heliosphere: Physical Processes in the Termination Shock and Heliosheath by Stone, E. C., Richardson, John D.

“…The solar wind evolves as it moves outward due to interactions with both itself and with the circum-heliospheric interstellar medium. The speed is, on average, constant out to 30 AU, then starts a slow decrease due to the pickup of interstellar neutrals. …”
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The solar wind in the outer heliosphere by Richardson, John D., Stone, E. C.

“…The solar wind evolves as it moves outward due to interactions with both itself and with the circum-heliospheric interstellar medium. The speed is, on average, constant out to 30 AU, then starts a slow decrease due to the pickup of interstellar neutrals. …”
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USING THE X-RAY DUST SCATTERING HALO OF CYGNUS X-1 TO DETERMINE DISTANCE AND DUST DISTRIBUTIONS by Xiang, Jingen, Lee, Julia C., Nowak, Michael A., Wilms, Jörn

“…Using 18 different dust models, including one modified by us (eponymously dubbed XLNW), we probe the interstellar medium between us and this source. A consistent description of the cloud properties along the line of sight (LOS) that describes at the same time the halo radial profile, the halo light curves, and the column density from source spectroscopy is best achieved with a small subset of these models. …”
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TRIANGULATION OF THE INTERSTELLAR MAGNETIC FIELD by Schwadron, N. A., Burlaga, L. F., McComas, David J., Mobius, Eberhard, Richardson, John D.

“…Determining the direction of the local interstellar magnetic field (LISMF) is important for understanding the heliosphere's global structure, the properties of the interstellar medium, and the propagation of cosmic rays in the local galactic medium. …”
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First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback by Nelson, Dylan, Pillepich, Annalisa, Springel, Volker, Pakmor, Rüdiger, Weinberger, Rainer, Genel, Shy, Torrey, Paul, Vogelsberger, Mark, Marinacci, Federico, Hernquist, Lars

“…The median spatial resolution of star-forming interstellar medium gas is ∼100−140 pc. This resolution approaches or exceeds that of modern 'zoom' simulations of individual massive galaxies, while the volume contains ∼20 000 resolved galaxies with M* ≳ 107 M☉. …”
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The evolution of the mass-metallicity relation and its scatter in IllustrisTNG by Torrey, Paul, Vogelsberger, Mark, Marinacci, Federico, Pakmor, Rüdiger, Springel, Volker, Nelson, Dylan, Naiman, Jill, Pillepich, Annalisa, Genel, Shy, Weinberger, Rainer, Hernquist, Lars

“…Our simulations indicate that the metal retention efficiency of the interstellar medium (ISM) is low: a majority of gas-phase metals ($\sim$ 85 per cent at $z=0$) live outside of the ISM, either in an extended gas disk, the circumgalactic medium, or outside the halo. …”
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PARSEC-SCALE BIPOLAR X-RAY SHOCKS PRODUCED BY POWERFUL JETS FROM THE NEUTRON STAR CIRCINUS X-1 by Sell, P. H., Heinz, Sebastian, Calvelo-Santos, D. E., Tudose, V., Soleri, P., Fender, R. P., Jonker, P. G., Brandt, W. N., Wijnands, R., van der Klis, M., Casella, P., Schulz, Norbert S., Nowak, Michael A.

“…The morphology of the emission regions suggests that the jets from Circinus X-1 are running into a terminal shock with the interstellar medium, as is seen in powerful radio galaxies. …”
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A redshift-dependent IRX–β dust attenuation relation for TNG50 galaxies by Schulz, Sebastian, Popping, Gergö, Pillepich, Annalisa, Nelson, Dylan, Vogelsberger, Mark, Marinacci, Federico, Hernquist, Lars

“…We select 7280 star-forming main-sequence (SFMS) galaxies with stellar mass ≥109 M⊙ at redshifts 0 ≤ z ≤ 4 and perform radiative transfer with skirt to model effects of interstellar medium dust on the emitted stellar light. Assuming a Milky Way dust type and a dust-to-metal ratio of 0.3, we find that TNG50 SFMS galaxies generally agree with observationally derived IRX-β relations at z ≳ 1. …”
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