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Journal articles on the topic 'Hot flows'

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Published: 4 June 2021
Last updated: 8 February 2022

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1

Mathews, W. G., and M. Loewenstein. "Hot galactic flows." Astrophysical Journal 306 (July 1986): L7. http://dx.doi.org/10.1086/184693.

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2

Yuan, Feng, Defu Bu, and Maochun Wu. "Outflow from Hot Accretion Flows." Proceedings of the International Astronomical Union 8, S290 (August 2012): 86–89. http://dx.doi.org/10.1017/s1743921312019278.

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AbstractNumerical simulations of hot accretion flows have shown that the mass accretion rate decreases with decreasing radius. Two models have been proposed to explain this result. In the adiabatic inflow-outflow solution (ADIOS), it is thought to be due to the loss of gas in outflows. In the convection-dominated accretion flow (CDAF) model, it is explained as because that the gas is locked in convective eddies. In this paper we use hydrodynamical (HD) and magnetohydrodynamical (MHD) simulations to investigate which one is physical. We calculate and compare various properties of inflow (gas with an inward velocity) and outflow (gas with an outward velocity). Systematic and significant differences are found. For example, for HD flows, the temperature of outflow is higher than inflow; while for MHD flows, the specific angular momentum of outflow is much higher than inflow. We have also analyzed the convective stability of MHD accretion flow and found that they are stable. These results suggest that systematic inward and outward motion must exist, i.e., the ADIOS model is favored. The different properties of inflow and outflow also suggest that the mechanisms of producing outflow in HD and MHD flows are buoyancy associated with the convection and the centrifugal force associated with the angular momentum transport mediated by the magnetic field, respectively. The latter mechanism is similar to the Blandford & Payne mechanism but no large-scale open magnetic field is required here. Possible observational applications are briefly discussed.
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3

Loewenstein, Michael, and William G. Mathews. "Evolution of hot galactic flows." Astrophysical Journal 319 (August 1987): 614. http://dx.doi.org/10.1086/165482.

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4

Ghasemnezhad, Maryam, and Maryam Samadi. "Radial Convection in Hot Accretion Flows." Astrophysical Journal 865, no. 2 (September 26, 2018): 93. http://dx.doi.org/10.3847/1538-4357/aad8af.

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5

Yan, Cheng. "Hot money in disaggregated capital flows." European Journal of Finance 24, no. 14 (December 13, 2017): 1190–223. http://dx.doi.org/10.1080/1351847x.2017.1411821.

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6

Bruun, H. H. "Hot-film anemometry in liquid flows." Measurement Science and Technology 7, no. 10 (October 1, 1996): 1301–12. http://dx.doi.org/10.1088/0957-0233/7/10/003.

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7

Yuan, Feng, Ronald E. Taam, Yongquan Xue, and Wei Cui. "Hot One‐Temperature Accretion Flows Revisited." Astrophysical Journal 636, no. 1 (January 2006): 46–55. http://dx.doi.org/10.1086/497980.

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8

Renzini, Alvio. "Hot Gas Flows in Elliptical Galaxies." Symposium - International Astronomical Union 171 (1996): 131–38. http://dx.doi.org/10.1017/s0074180900232257.

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Stars in elliptical galaxies lose mass at an overall present rate Ṁ∗ ≃ 1.5 × 10−11LBM⊙yr−1 (e.g., Faber & Gallagher 1976; Renzini & Buzzoni 1986). When allowing for the predicted increase back with cosmological time it turns out that over one Hubble time the stellar population of an elliptical galaxy has cumulatively lost 20-50% of its initial mass, the precise value depending on the IMF. This review focuses on two simple questions: what happens to the gas being lost by the stars? Where is it ultimately disposed?
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9

Sharma, Prateek, Eliot Quataert, Gregory W. Hammett, and James M. Stone. "Electron Heating in Hot Accretion Flows." Astrophysical Journal 667, no. 2 (October 2007): 714–23. http://dx.doi.org/10.1086/520800.

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10

Zakamska, Nadia L., Mitchell C. Begelman, and Roger D. Blandford. "Hot Self‐Similar Relativistic Magnetohydrodynamic Flows." Astrophysical Journal 679, no. 2 (June 2008): 990–99. http://dx.doi.org/10.1086/587870.

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11

Xie, Fu-Guo, and Feng Yuan. "Radiative efficiency of hot accretion flows." Monthly Notices of the Royal Astronomical Society 427, no. 2 (November 19, 2012): 1580–86. http://dx.doi.org/10.1111/j.1365-2966.2012.22030.x.

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12

Yuan, Feng, and Ramesh Narayan. "Hot Accretion Flows Around Black Holes." Annual Review of Astronomy and Astrophysics 52, no. 1 (August 18, 2014): 529–88. http://dx.doi.org/10.1146/annurev-astro-082812-141003.

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13

Claessens, Stijn, Michael P. Dooley, and Andrew Warner. "Portfolio Capital Flows: Hot or Cold?" World Bank Economic Review 9, no. 1 (1995): 153–74. http://dx.doi.org/10.1093/wber/9.1.153.

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14

Hinz, Denis F., Simon Graner, and Christian Breitsamter. "Stratification in hot water pipe-flows." Energy Procedia 116 (June 2017): 324–33. http://dx.doi.org/10.1016/j.egypro.2017.05.079.

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15

Gross, A., and C. Weiland. "Numerical Simulation of Hot Gas Nozzle Flows." Journal of Propulsion and Power 20, no. 5 (September 2004): 879–91. http://dx.doi.org/10.2514/1.5001.

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16

Kirk, Daniel R., Douglas O. Creviston, and Ian A. Waitz. "Aeroacoustic Measurement of Transient Hot Nozzle Flows." Journal of Propulsion and Power 17, no. 4 (July 2001): 928–35. http://dx.doi.org/10.2514/2.5826.

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17

Niedźwiecki, Andrzej, Fu-Guo Xie, and Agnieszka Stȩpnik. "X-ray emission from hot accretion flows." Proceedings of the International Astronomical Union 9, S304 (October 2013): 266–69. http://dx.doi.org/10.1017/s1743921314004037.

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AbstractRadiatively inefficient, hot accretion flows are widely considered as a relevant accretion mode in low-luminosity AGNs. We study spectral formation in such flows using a refined model with a fully general relativistic description of both the radiative (leptonic and hadronic) and hydrodynamic processes, as well as with an exact treatment of global Comptonization. We find that the X-ray spectral index–Eddington ratio anticorrelation as well as the cut-off energy measured in the best-studied objects favor accretion flows with rather strong magnetic field and with a weak direct heating of electrons. Furthermore, they require a much stronger source of seed photons than considered in previous studies. The nonthermal synchrotron radiation of relativistic electrons seems to be the most likely process capable of providing a sufficient flux of seed photons. Hadronic processes, which should occur due to basic properties of hot flows, provide an attractive explanation for the origin of such electrons.
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18

Menou, Kristen. "Hot Jupiter atmospheric flows at high resolution." Monthly Notices of the Royal Astronomical Society 493, no. 4 (February 24, 2020): 5038–44. http://dx.doi.org/10.1093/mnras/staa532.

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ABSTRACT Global circulation models (GCMs) of atmospheric flows are now routinely used to interpret observational data on hot Jupiters. Localized ‘equatorial β-plane’ simulations have revealed that a barotropic (horizontal shear) instability of the equatorial jet appears at horizontal resolutions beyond those typically achieved in global models; this instability could limit wind speeds and lead to increased atmospheric variability. To address this possibility, we adapt the computationally efficient, pseudo-spectral PlaSim GCM, originally designed for Earth studies, to model hot Jupiter atmospheric flows and validate it on a reference benchmark. We then present high-resolution global models of HD209458b, with horizontal resolutions of T85 (128×256) and T127 (192×384). The barotropic instability phenomenology found in β-plane simulations is not reproduced in these global models, despite comparably high meridional resolutions. Nevertheless, high-resolution models do exhibit additional flow variability on long time-scales (of the order of 100 planet days or more), which is absent from the lower resolution models. It manifests as a breakdown of the north–south symmetry of the equatorial wind. By post-processing the atmospheric flows at various resolutions (assuming a cloud-free situation), we show that the stronger flow variability achieved at high resolution does not translate into noticeably stronger dayside infrared flux variability. More generally, our results suggest that high horizontal resolutions are not required to capture the key features of hot Jupiter atmospheric flows.
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19

Özel, Feryal, and Tiziana Di Matteo. "X‐Ray Images of Hot Accretion Flows." Astrophysical Journal 548, no. 1 (February 10, 2001): 213–18. http://dx.doi.org/10.1086/318658.

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20

Niedźwiecki, Andrzej, Fu-Guo Xie, and Agnieszka Stȩpnik. "X-ray spectra of hot accretion flows." Monthly Notices of the Royal Astronomical Society 443, no. 2 (July 25, 2014): 1733–47. http://dx.doi.org/10.1093/mnras/stu1262.

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21

Daley-Yates, S., and I. R. Stevens. "Interacting fields and flows: Magnetic hot Jupiters." Astronomische Nachrichten 338, no. 8 (October 2017): 881–84. http://dx.doi.org/10.1002/asna.201713395.

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22

Fabian, A. C. "X-ray Haloes and Cooling Flows." Symposium - International Astronomical Union 144 (1991): 237–44. http://dx.doi.org/10.1017/s0074180900089130.

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The properties of hot gaseous haloes in massive early-type galaxies are briefly reviewed. Gas flows in such haloes are complex yet so large-scale that they may guide us in the understanding of flows around disk galaxies. The intracluster medium is discussed as a further illustration of the properties of diffuse hot gas trapped in a gravtational well. Finally, the possibility of the existence of a significant diffuse medium in the Local Group, and in groups in general, is revived. Such a medium would generate a substantial disk-halo interaction with our Galaxy.
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23

Erofeeva, Natalya V., and Irina N. Chebotova. "MODELING BELT CONVEYOR OPERATION ON HOT CARGO FLOWS." Mining Equipment and Electromechanics 140, no. 6 (2019): 14–19. http://dx.doi.org/10.26730/1816-4528-2018-6-14-19.

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24

Bu, De-Fu, Feng Yuan, and James M. Stone. "Magnetothermal and magnetorotational instabilities in hot accretion flows." Monthly Notices of the Royal Astronomical Society 413, no. 4 (March 8, 2011): 2808–14. http://dx.doi.org/10.1111/j.1365-2966.2011.18354.x.

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25

Langton, Jonathan, and Gregory Laughlin. "Observational Consequences of Hydrodynamic Flows on Hot Jupiters." Astrophysical Journal 657, no. 2 (February 13, 2007): L113—L116. http://dx.doi.org/10.1086/513185.

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26

Davies, P. O. A. L. "Plane acoustic wave propagation in hot gas flows." Journal of Sound and Vibration 122, no. 2 (April 1988): 389–92. http://dx.doi.org/10.1016/s0022-460x(88)80362-6.

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27

Rauscher, Emily, and Kristen Menou. "THREE-DIMENSIONAL MODELING OF HOT JUPITER ATMOSPHERIC FLOWS." Astrophysical Journal 714, no. 2 (April 19, 2010): 1334–42. http://dx.doi.org/10.1088/0004-637x/714/2/1334.

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28

VISHNIAC, E. T. "Hot Halos: Cooling Flows in Clusters and Galaxies." Science 245, no. 4920 (August 25, 1989): 873–74. http://dx.doi.org/10.1126/science.245.4920.873-a.

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29

Esin, Ann A., Ramesh Narayan, Eve Ostriker, and Insu Yi. "Hot One-Temperature Accretion Flows around Black Holes." Astrophysical Journal 465 (July 1996): 312. http://dx.doi.org/10.1086/177421.

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30

Torregrosa, A. J., A. Broatch, J. García-Tíscar, and F. Roig. "Experimental verification of hydrodynamic similarity in hot flows." Experimental Thermal and Fluid Science 119 (November 2020): 110220. http://dx.doi.org/10.1016/j.expthermflusci.2020.110220.

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31

Cau, G., N. Mandas, G. Manfrida, and F. Nurzia. "Measurements of Primary and Secondary Flows in an Industrial Forward-Curved Centrifugal Fan." Journal of Fluids Engineering 109, no. 4 (December 1, 1987): 353–58. http://dx.doi.org/10.1115/1.3242671.

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An industrial-type centrifugal-flow fan was instrumented and tested in order to obtain a fully detailed relative flow pattern at impeller discharge. Testing entailed investigation of both primary flows (jet-wake pattern and presence of return flows) and secondary flows (due to streamwise vorticity either from meridional curvature or rotation effects). In addition to conventional probing, a crossed hot-wire probe was employed in the tests. Ensemble-averaging the hot-wire signals made it possible to obtain the three-dimensional phase-averaged relative flow pattern at discharge by means of double positioning of the probe. Results show secondary-flow effects of appreciable magnitude interacting with primary flows (e.g., return flow in the hub region and variations in vortex structure and wake position with variations in flowrate).
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32

Alben, S. "Optimal convection cooling flows in general 2D geometries." Journal of Fluid Mechanics 814 (February 8, 2017): 484–509. http://dx.doi.org/10.1017/jfm.2017.35.

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We generalize a recent method for computing optimal 2D convection cooling flows in a horizontal layer to a wide range of geometries, including those relevant for technological applications. We write the problem in a conformal pair of coordinates which are the pure conduction temperature and its harmonic conjugate. We find optimal flows for cooling a cylinder in an annular domain, a hot plate embedded in a cold surface, and a channel with a hot interior and cold exterior. With a constraint of fixed kinetic energy, the optimal flows are all essentially the same in the conformal coordinates. In the physical coordinates, they consist of vortices ranging in size from the length of the hot surface to a small cutoff length at the interface of the hot and cold surfaces. With the constraint of fixed enstrophy (or fixed rate of viscous dissipation), a geometry-dependent metric factor appears in the equations. The conformal coordinates are useful here because they map the problems to a rectangular domain, facilitating numerical solutions. With a small enstrophy budget, the optimal flows are dominated by vortices that have the same size as the flow domain.
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33

Brennan, Michael J., and Carmen Aranda. "What Makes Hot Money Hot? The Relative Volatility of International Flows of Debt and Equity Capital." Review of Pacific Basin Financial Markets and Policies 02, no. 04 (December 1999): 427–51. http://dx.doi.org/10.1142/s0219091599000230.

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This paper is concerned with the relative volatility of international flows of debt and equity capital. It is shown that if foreign investors are less well informed about the domestic economy than domestic investors, then international flows of debt capital will be more volatile than flows of equity capital in the sense that the proportional change of foreign bondholdings in an economy in response to a change in that economy's economic prospects will be greater than the proportional change in foreign stockholdings. This is shown to be consistent with the behavior of international flows of debt and equity capital during the Asian crisis.
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34

Pellegrini, Silvia. "Hot gas flows on global and nuclear galactic scales." Proceedings of the International Astronomical Union 5, H15 (November 2009): 277. http://dx.doi.org/10.1017/s1743921310009208.

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AbstractOne of the most significant observational improvements allowed by the high quality Chandra data of galaxies is the measurement of the nuclear luminosities down to low values, and of the hot ISM properties down to very low gas contents. I present here some recent developements concerning the possibility of accreting and outflowing gas, based on modeling results that take into account the role of a central supermassive black hole (MBH).
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35

Kafexhiu, E., F. Aharonian, and M. Barkov. "Nuclear γ-ray emission from very hot accretion flows." Astronomy & Astrophysics 623 (March 2019): A174. http://dx.doi.org/10.1051/0004-6361/201833948.

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Optically thin accretion plasmas can reach ion temperatures Ti ≥ 1010 K and thus trigger nuclear reactions. Using a large nuclear interactions network, we studied the radial evolution of the chemical composition of the accretion flow toward the black hole and computed the emissivity in nuclear γ-ray lines. In the advection dominated accretion flow (ADAF) regime, CNO and heavier nuclei are destroyed before reaching the last stable orbit. The overall luminosity in the de-excitation lines for a solar composition of plasma can be as high as few times 10−5 the accretion luminosity (Ṁc2) and can be increased for heavier compositions up to 10−3. The efficiency of transformation of the kinetic energy of the outflow into high energy (≥100 MeV) γ-rays through the production and decay of π0-mesons can be higher, up to 10−2 of the accretion luminosity. We show that in the ADAF model up to 15% of the mass of accretion matter can “evaporate” in the form of neutrons.
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36

Yuan, Feng, and De-Fu Bu. "On the convective instability of hot radiative accretion flows." Monthly Notices of the Royal Astronomical Society 408, no. 2 (July 26, 2010): 1051–60. http://dx.doi.org/10.1111/j.1365-2966.2010.17175.x.

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37

Cai, Tao, Vinh Q. T. Dang, and Jennifer T. Lai. "China's Capital and ‘Hot’ Money Flows: An Empirical Investigation." Pacific Economic Review 21, no. 3 (March 19, 2016): 276–94. http://dx.doi.org/10.1111/1468-0106.12091.

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38

Zhang, Yihao, Fang Chen, Jian Huang, and Catherine Shenoy. "Hot money flows and production uncertainty: Evidence from China." Pacific-Basin Finance Journal 57 (October 2019): 101070. http://dx.doi.org/10.1016/j.pacfin.2018.09.006.

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39

Yuan, Feng, Fuguo Xie, and Jeremiah P. Ostriker. "GLOBAL COMPTON HEATING AND COOLING IN HOT ACCRETION FLOWS." Astrophysical Journal 691, no. 1 (January 7, 2009): 98–104. http://dx.doi.org/10.1088/0004-637x/691/1/98.

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40

Koval, A., J. Šafránková, and Z. Němeček. "A study of particle flows in hot flow anomalies." Planetary and Space Science 53, no. 1-3 (January 2005): 41–52. http://dx.doi.org/10.1016/j.pss.2004.09.027.

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41

Dalla Vecchia, Claudio, Richard G. Bower, Tom Theuns, Michael L. Balogh, Pasquale Mazzotta, and Carlos S. Frenk. "Quenching cluster cooling flows with recurrent hot plasma bubbles." Monthly Notices of the Royal Astronomical Society 355, no. 3 (December 11, 2004): 995–1004. http://dx.doi.org/10.1111/j.1365-2966.2004.08381.x.

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42

Bu, De-Fu, and Xiao-Hong Yang. "Thermal wind from hot accretion flows at large radii." Monthly Notices of the Royal Astronomical Society 476, no. 4 (January 9, 2018): 4395–402. http://dx.doi.org/10.1093/mnras/sty053.

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43

Fukumura, Keigo, and Demosthenes Kazanas. "Mass Outflows from Dissipative Shocks in Hot Accretion Flows." Astrophysical Journal 669, no. 1 (November 2007): 85–95. http://dx.doi.org/10.1086/521578.

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44

Wu, MaoChun, Feng Yuan, and DeFu Bu. "Numerical simulation of hot accretion flows with thermal conduction." Science China Physics, Mechanics and Astronomy 53, S1 (January 2010): 168–72. http://dx.doi.org/10.1007/s11433-010-0037-x.

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45

Kai, Yun, Walter Garen, David E. Zeitoun, and Ulrich Teubner. "Formation and hot flow duration of micro shock flows." Physics of Fluids 30, no. 7 (July 2018): 072001. http://dx.doi.org/10.1063/1.5023475.

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46

Quataert, Eliot. "Particle Heating by Alfvenic Turbulence in Hot Accretion Flows." Astrophysical Journal 500, no. 2 (June 20, 1998): 978–91. http://dx.doi.org/10.1086/305770.

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47

Song, Justin C. W., and Leonid S. Levitov. "Energy flows in graphene: hot carrier dynamics and cooling." Journal of Physics: Condensed Matter 27, no. 16 (April 2, 2015): 164201. http://dx.doi.org/10.1088/0953-8984/27/16/164201.

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48

Cutler, A. D., and P. Bradshaw. "A crossed hot-wire technique for complex turbulent flows." Experiments in Fluids 12-12, no. 1-2 (December 1991): 17–22. http://dx.doi.org/10.1007/bf00226561.

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49

Briassulis, G., A. Honkan, J. Andreopoulos, and C. B. Watkins. "Application of hot-wire anemometry in shock-tube flows." Experiments in Fluids 19, no. 1 (May 1995): 29–37. http://dx.doi.org/10.1007/bf00192230.

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50

Ozel, Feryal, Dimitrios Psaltis, and Ramesh Narayan. "Hybrid Thermal‐Nonthermal Synchrotron Emission from Hot Accretion Flows." Astrophysical Journal 541, no. 1 (September 20, 2000): 234–49. http://dx.doi.org/10.1086/309396.

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