Cited by 714Astrophysics and Star Formation StudiesGalaxies: Formation, Evolution, PhenomenaAstrophysical Phenomena and Observations

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Consequences of a New Hot Component of the Interstellar Medium

Shapiro, Paul R., Field, George B.·1976·The Astrophysical Journal

DOI 10.1086/154332

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Abstract

The suggestion that the observed 0.25 keV X-ray background and O VI sabsorption lines are produced by a new, hot (T∼106 K), diffuse component of the medium is examined in the context of both a steady-state and a time-dependent model. It is concluded that such a component can explain the two observations only if (1) the pressure of the cooler interstellar medium is 10 times higher than the previously estimated p/k∼2000 cm-3K; (2) a mechanism such as the proposed convective-radiative "galactic fountain" exists to cool the hot gas; and (3) another component is responsible for the presence of O VI at temperatures below 106 K. Subject headings: interstellar: matter - X-rays: general

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Background
Mass and Energy Balance in the Interstellar Medium: How to Model the Disk Gas in our Galaxy
Cowie, L. L. (1987) · Astrophysics and space science library · doi:10.1007/978-94-009-3861-8_11 · Cited by 6
Final Size of a Magnetized Superbubble
Kamaya, H. (1998) · The Astrophysical Journal · doi:10.1086/311145 · Cited by 6
Disc galaxy evolution along the Hubble sequence
Kampakoglou, M., & Silk, J. I. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12099.x · Cited by 6
“Models of gas flow on the galactic scale were first introduced by Shapiro & Field (1976) and subsequently developed by Bregman (1980) and others.”
Method
Low and high velocity clouds produced by young stellar clusters
Rodríguez-González, A., Raga, A. C., & Cantó, J. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200911693 · Cited by 6
“These models were described by Shapiro & Field (1976), Houck & Bregman (1990), and de Gouveia Dal Pino et al. (2009).”
Method
Hot Gas in the Disk, Halo, and Disk-Halo Interaction
Cox, D. P. (1991) · Springer eBooks · doi:10.1007/978-94-011-3228-2_15 · Cited by 6
The Interstellar Medium Near the Sun
Bruhweiler, F. C., & Vidal‐Madjar, A. (1987) · Astrophysics and space science library · doi:10.1007/978-94-009-3753-6_20 · Cited by 6
H i and optical spectroscopy towards the M15 intermediate-velocity cloud
Smoker, J. V., Lehner, N., Keenan, F. P., et al. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.03999.x · Cited by 6
How the Galaxy keeps its halo
Shull, J. M. (1996) · Nature · doi:10.1038/380668a0 · Cited by 6
The Impact of Cosmic Ray Injection on Magnetic Flux Tubes in a Galactic Disk
Habegger, R., Zweibel, E. G., & Wong, S. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/accf8e · Cited by 5
The SAMI Galaxy Survey: ΣSFR drives the presence of complex emission-line profiles in star-forming galaxies
Zovaro, H. R. M., Mendel, J. T., Groves, B. A., Kewley, L. J., Colless, M., Ristea, A., Cortese, L., Oh, S., D’Eugenio, F., Croom, S. M., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3747 · Cited by 5
Properties of 3D H i filaments in the smith high velocity cloud
Holm-Hansen, C., Putman, M. E., & Kim, D. A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2801 · Cited by 6
The Plane Quasar Survey: First Data Release
Werk, J., Tchernyshyov, K., Bish, H., Zheng, Y., Putman, M., Peek, J., & Schiminovich, D. (2024) · Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad58df · Cited by 7
“…of this material are generally thought to be consistent with gas cycling in a Galactic fountain, in which hot, overpressurized gas ﬂ ows from the disk into the halo, and subsequently cools, recombines, and rains back down onto the disk ( e.g., Shapiro & Field 1976; Fraternali & Binney 2008 ) .”
A NEW DELIVERY ROUTE TO GALACTIC NUCLEI: WARM HALO CLOUD IMPACTS
McKernan, B., Maller, A. H., & Ford, K. E. S. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/718/2/l83 · Cited by 5
“Around our Galaxy, two basic models can account for the properties of observed high velocity clouds (HVCs): an accretion model based on WHCs (e.g. Blitz et al. 1999; Maller & Bullock 2004) or a Galactic fountain model (Shapiro & Field 1976).”
Method
A population of high-velocity absorption-line systems residing in the Local Group
Bouma, S., Richter, P., & Fechner, C. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935078/pdf · Cited by 5
Non-equilibrium ionisation plasmas in the interstellar medium
Breitschwerdt, D., & de Avillez, M. A. (2021) · Astrophysics and Space Science · doi:10.1007/s10509-021-03993-9 · Cited by 5
“Some of the material blown out into the halo might rain down again in form of a Galactic fountain (Shapiro and Field 1976; Bregman 1980; Kahn 1981; de Avillez 2000).”
Background
The Impact of Space Experiments on our Knowledge of the Physics of the Universe
Giovannelli, F., & Sabau-Graziati, L. (2004) · Space Science Reviews · doi:10.1023/b:spac.0000032807.99883.09 · Cited by 5
Discovery of the Goat Horn complex: a ∼1000 deg2 diffuse X-ray source connected to radio loop XII
Locatelli, N. T., Ponti, G., Merloni, A., Zheng, X., Dennerl, K., Haberl, F., Maitra, C., Sanders, J. S., Sasaki, M., & Zhang, H. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449356 · Cited by 5
Seeking edge-on galaxies with substantial extraplanar dust using a radiative transfer model: determination of the model parameter uncertainties for EON_10.477_41.954 (FGC 79)
Shinn, J. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2442 · Cited by 5
“They include hydrodynamic phenomena such as galactic fountain flows (Shapiro & Field 1976; Bregman 1980; Houck & Bregman 1990), radiation pressure (Ferrara et al. ?”
Background
Solar-metallicity gas in the extended halo of a galaxy at z ∼ 0.12
Pradeep, J., Sankar, S., Umasree, T. M., Narayanan, A., Khaire, V., Gebhardt, M., Sameer, S., & Charlton, J. C. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa184 · Cited by 5
“…velocities of 30 km s−1 < ∆v < 90 km s−1 relative to the LSR, are presumed to be interstellar gas expelled from the disk as galactic fountains powered by supernova events (Shapiro & Field 1976, Bregman 1980, Norman & Ikeuchi 1989, Houck & Bregman 1990, Richter et al. 2001c, Sarkar et al. 2017).”
Background
The Origin of the High-velocity Clouds
Bregman, J. N. (2004) · Springer eBooks · doi:10.1007/1-4020-2579-3_16 · Cited by 5

Authors: Shapiro, P. R., & Field, G. B.
ORCID: Shapiro, Paul R.
Venue: The Astrophysical Journal
Publisher: American Astronomical Society
Published: 1976-05
Volume: 205
Pages: 762
ISSN: 0004-637X (ISSN-L)
1538-4357
DOI: 10.1086/154332
OpenAlex: W2046029142
Cited by: 714
References: 0
Citations by year: 2026: 10 · 2025: 19 · 2024: 23 · 2023: 18 · 2022: 20 · 2021: 13 · 2020: 16 · 2019: 30 · 2018: 15 · 2017: 22 · 2016: 32 · 2015: 13 · 2014: 15 · 2013: 18 · 2012: 33
FWCI: 8.82
Type: journal article
Language: en
Open access: closed
Locations: The Astrophysical Journal (publishedVersion)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Keywords: hot interstellar medium, interstellar medium pressure, Galactic fountain, hot gas cooling, interstellar medium, steady-state model, time-dependent model

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Consequences of a New Hot Component of the Interstellar Medium

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