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Gotowe bibliografie tematyczne / Galactic Outflow

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Gotowa bibliografia na temat „Galactic Outflow”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Galactic Outflow"

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Tanner, Ryan, i Kimberly A. Weaver. "Simulations of AGN-driven Galactic Outflow Morphology and Content". Astronomical Journal 163, nr 3 (17.02.2022): 134. http://dx.doi.org/10.3847/1538-3881/ac4d23.

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Abstract Using a series of 3D relativistic hydrodynamical simulations of active galactic nuclei (AGN) we investigate how AGN power, a clumpy interstellar medium (ISM) structure, and AGN jet angle with respect to the galactic disk affect the morphology and content of the resulting galactic outflow. For low-power AGN across three orders of magnitude of AGN luminosities (1041–1043 erg s−1) our simulations did not show significant changes to either the morphology or total mass of the outflow. Changing the angle of the AGN jet with respect to the galaxy did show small changes in the total outflow mass of a factor of 2–3. Jets perpendicular to the galactic disk created hot single-phase outflows, while jets close to parallel with the disk created multiphase outflows with equal parts warm and hot, and significant cold gas. Overall the final morphology of low-power AGN outflows depends primarily on how the jet impacts and interacts with large, dense clouds in the clumpy ISM. These clouds can disrupt, deflect, split, or suppress the jet, preventing it from leaving the galactic disk as a coherent structure. But for simulations with AGN luminosities > 1044 erg s−1 the ISM played a minor role in determining the morphology of the outflow with an undisrupted jet leaving the disk. The final morphology of AGN outflows is different for low-power AGNs versus high-power AGNs with the final morphology of low-power AGN outflows dependent on the ISM structure within the first kiloparsec surrounding the AGN.

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Wu, Kinwah, Kaye Jiale Li, Ellis R. Owen, Li Ji, Shuinai Zhang i Graziella Branduardi-Raymont. "Charge-exchange emission and cold clumps in multiphase galactic outflows". Monthly Notices of the Royal Astronomical Society 491, nr 4 (26.11.2019): 5621–35. http://dx.doi.org/10.1093/mnras/stz3301.

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ABSTRACT Large-scale outflows from starburst galaxies are multiphase, multicomponent fluids. Charge-exchange lines that originate from the interfacing surface between the neutral and ionized components are a useful diagnostic of the cold dense structures in the galactic outflow. From the charge-exchange lines observed in the nearby starburst galaxy M82, we conduct surface-to-volume analyses and deduce that the cold dense clumps in its galactic outflow have flattened shapes, resembling a hamburger or a pancake morphology rather than elongated shapes. The observed filamentary H α features are therefore not prime charge-exchange line emitters. They are stripped material torn from the slow-moving dense clumps by the faster moving ionized fluid, which are subsequently warmed and stretched into elongated shapes. Our findings are consistent with numerical simulations that have shown that cold dense clumps in galactic outflows can be compressed by ram pressure, and also progressively ablated and stripped before complete disintegration. We have shown that some clumps could survive their passage along a galactic outflow. These are advected into the circumgalactic environment, where their remnants would seed condensation of the circumgalactic medium to form new clumps. The infall of these new clumps back into the galaxy and their subsequent re-entrainment into the galactic outflow form a loop process of galactic material recycling.

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Fluetsch, A., R. Maiolino, S. Carniani, S. Arribas, F. Belfiore, E. Bellocchi, S. Cazzoli i in. "Properties of the multiphase outflows in local (ultra)luminous infrared galaxies". Monthly Notices of the Royal Astronomical Society 505, nr 4 (14.06.2021): 5753–83. http://dx.doi.org/10.1093/mnras/stab1666.

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ABSTRACT Galactic outflows are known to consist of several gas phases; however, the connection between these phases has been investigated little and only in a few objects. In this paper, we analyse Multi Unit Spectroscopic Explorer (MUSE)/Very Large Telescope (VLT) data of 26 local (U)LIRGs and study their ionized and neutral atomic phases. We also include objects from the literature to obtain a sample of 31 galaxies with spatially resolved multiphase outflow information. We find that the ionized phase of the outflows has on average an electron density three times higher than the disc (ne,disc ∼ 145 cm−3 versus ne,outflow ∼ 500 cm−3), suggesting that cloud compression in the outflow is more important than cloud dissipation. We find that the difference in extinction between outflow and disc correlates with the outflow gas mass. Together with the analysis of the outflow velocities, this suggests that at least some of the outflows are associated with the ejection of dusty clouds from the disc. This may support models where radiation pressure on dust contributes to driving galactic outflows. The presence of dust in outflows is relevant for potential formation of molecules inside them. We combine our data with millimetre data to investigate the molecular phase. We find that the molecular phase accounts for more than 60 ${{\ \rm per\ cent}}$ of the total mass outflow rate in most objects and this fraction is higher in active galactic nuclei (AGN)-dominated systems. The neutral atomic phase contributes of the order of 10 ${{\ \rm per\ cent}}$, while the ionized phase is negligible. The ionized-to-molecular mass outflow rate declines slightly with AGN luminosity, although with a large scatter.

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Mao, Junjie. "Density diagnostics of photoionized outflows in active galactic nuclei". Proceedings of the International Astronomical Union 15, S350 (kwiecień 2019): 274–77. http://dx.doi.org/10.1017/s1743921319007750.

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AbstractPhotoionized outflows in active galactic nuclei (AGNs) are thought to influence their circumnuclear and host galactic environment. However, the distance of the outflow with respect to the black hole is poorly constrained, which limits our understanding of the kinetic power by the outflow. Therefore, the impact of AGN outflows on their host galaxies is uncertain. If the density of the outflow is known, its distance can be derived. Density measurement via variability studies and density sensitive lines have been used, albeit not very effective in the X-ray band. Good measurements are rather demanding or challenging for the current generation of (grating) spectrometers. The next generation of spectrometers will certainly provide data with better quality and large quantity, leading to tight constraints on the location and the kinetic power of AGN outflows. This contribution summarizes the state-of-the-art in this field.

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Ishibashi, W., A. C. Fabian i N. Arakawa. "AGN-driven galactic outflows: comparing models to observations". Monthly Notices of the Royal Astronomical Society 502, nr 3 (30.01.2021): 3638–45. http://dx.doi.org/10.1093/mnras/stab266.

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ABSTRACT The actual mechanism(s) powering galactic outflows in active galactic nuclei (AGNs) is still a matter of debate. At least two physical models have been considered in the literature: wind shocks and radiation pressure on dust. Here, we provide a first quantitative comparison of the AGN radiative feedback scenario with observations of galactic outflows. We directly compare our radiation pressure-driven shell models with the observational data from the most recent compilation of molecular outflows on galactic scales. We show that the observed dynamics and energetics of galactic outflows can be reproduced by AGN radiative feedback, with the inclusion of radiation trapping and/or luminosity evolution. The predicted scalings of the outflow energetics with AGN luminosity can also quantitatively account for the observational scaling relations. Furthermore, sources with both ultrafast and molecular outflow detections are found to be located in the ‘forbidden’ region of the NH–λ plane. Overall, an encouraging agreement is obtained over a wide range of AGN and host galaxy parameters. We discuss our results in the context of recent observational findings and numerical simulations. In conclusion, AGN radiative feedback is a promising mechanism for driving galactic outflows that should be considered, alongside wind feedback, in the interpretation of future observational data.

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Tokuda, Kazuki, Sarolta Zahorecz, Yuri Kunitoshi, Kosuke Higashino, Kei E. I. Tanaka, Ayu Konishi, Taisei Suzuki i in. "The First Detection of a Protostellar CO Outflow in the Small Magellanic Cloud with ALMA". Astrophysical Journal Letters 936, nr 1 (26.08.2022): L6. http://dx.doi.org/10.3847/2041-8213/ac81c1.

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Abstract Protostellar outflows are one of the most outstanding features of star formation. Observational studies over the last several decades have successfully demonstrated that outflows are ubiquitously associated with low- and high-mass protostars in solar-metallicity Galactic conditions. However, the environmental dependence of protostellar outflow properties is still poorly understood, particularly in the low-metallicity regime. Here we report the first detection of a molecular outflow in the Small Magellanic Cloud with 0.2 Z ⊙, using Atacama Large Millimeter/submillimeter Array observations at a spatial resolution of 0.1 pc toward the massive protostar Y246. The bipolar outflow is nicely illustrated by high-velocity wings of CO(3–2) emission at ≳15 km s−1. The evaluated properties of the outflow (momentum, mechanical force, etc.) are consistent with those of the Galactic counterparts. Our results suggest that the molecular outflows, i.e., the guidepost of the disk accretion at the small scale, might be universally associated with protostars across the metallicity range of ∼0.2–1 Z ⊙.

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Mitchell, Peter D., Joop Schaye, Richard G. Bower i Robert A. Crain. "Galactic outflow rates in the EAGLE simulations". Monthly Notices of the Royal Astronomical Society 494, nr 3 (9.04.2020): 3971–97. http://dx.doi.org/10.1093/mnras/staa938.

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ABSTRACT We present measurements of galactic outflow rates from the eagle suite of cosmological simulations. We find that gas is removed from the interstellar medium (ISM) of central galaxies with a dimensionless mass loading factor that scales approximately with circular velocity as $V_{\mathrm{c}}^{-3/2}$ in the low-mass regime where stellar feedback dominates. Feedback from active galactic nuclei causes an upturn in the mass loading for halo masses ${\gt}10^{12} \, \mathrm{M_\odot }$. We find that more gas outflows through the halo virial radius than is removed from the ISM of galaxies, particularly at low redshifts, implying substantial mass loading within the circumgalactic medium. Outflow velocities span a wide range at a given halo mass/redshift, and on average increase positively with redshift and halo mass up to $M_{200} \sim 10^{12} \, \mathrm{M_\odot }$. Outflows exhibit a bimodal flow pattern on circumgalactic scales, aligned with the galactic minor axis. We present a number of like-for-like comparisons to outflow rates from other recent cosmological hydrodynamical simulations, and show that comparing the propagation of galactic winds as a function of radius reveals substantial discrepancies between different models. Relative to some other simulations, eagle favours a scenario for stellar feedback where agreement with the galaxy stellar mass function is achieved by removing smaller amounts of gas from the ISM, but with galactic winds that then propagate and entrain ambient gas out to larger radii.

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Takasao, Shinsuke, Yuri Shuto i Keiichi Wada. "Spontaneous Formation of Outflows Powered by Rotating Magnetized Accretion Flows in a Galactic Center". Astrophysical Journal 926, nr 1 (1.02.2022): 50. http://dx.doi.org/10.3847/1538-4357/ac38a8.

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Abstract We investigate how magnetically driven outflows are powered by a rotating, weakly magnetized accretion flow onto a supermassive black hole using axisymmetric magnetohydrodynamic simulations. Our proposed model focuses on the accretion dynamics on an intermediate scale between the Schwarzschild radius and the galactic scale, which is ∼1–100 pc. We demonstrate that a rotating disk formed on a parsec-scale acquires poloidal magnetic fields via accretion, and this produces an asymmetric bipolar outflow at some point. The formation of the outflow was found to follow the growth of strongly magnetized regions around disk surfaces (magnetic bubbles). The bipolar outflow grew continuously inside the expanding bubbles. We theoretically derived the growth condition of the magnetic bubbles for our model that corresponds to a necessary condition for outflow growth. We found that the north–south asymmetrical structure of the bipolar outflow originates from the complex motions excited by accreting flows around the outer edge of the disk. The bipolar outflow comprises multiple mini-outflows and downflows (failed outflows). The mini-outflows emanate from the magnetic concentrations (magnetic patches). The magnetic patches exhibit inward drifting motions, thereby making the outflows unsteady. We demonstrate that the inward drift can be modeled using a simple magnetic patch model that considers magnetic angular momentum extraction. This study could be helpful for understanding how asymmetric and nonsteady outflows with complex substructures are produced around supermassive black holes without the help of strong radiation from accretion disks or entrainment by radio jets such as molecular outflows in radio-quiet active galactic nuclei, e.g., NGC 1377.

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Barai, Paramita. "How to Simulate Galactic Outflows?" Proceedings of the International Astronomical Union 10, S309 (lipiec 2014): 300–301. http://dx.doi.org/10.1017/s1743921314009971.

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AbstractA challenge in cosmological simulations is to formulate a physical model of star-formation (SF) and supernovae (SN) feedback which produces galactic outflows like that widely observed. In several models an outflow velocity (vout) and mass loading factor (η) are input to the sub-resolution recipe. We present results from our MUPPI model, which uses local properties of gas, and is able to develop galactic outflows whose properties correlate with global galaxy properties, consistent with observations; demonstrating a significant improvement in such work.

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Avery, Charlotte R., Stijn Wuyts, Natascha M. Förster Schreiber, Carolin Villforth, Caroline Bertemes, Wenjun Chang, Stephen L. Hamer, Jun Toshikawa i Junkai Zhang. "Incidence, scaling relations and physical conditions of ionized gas outflows in MaNGA". Monthly Notices of the Royal Astronomical Society 503, nr 4 (19.03.2021): 5134–60. http://dx.doi.org/10.1093/mnras/stab780.

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ABSTRACT In this work, we investigate the strength and impact of ionized gas outflows within z ∼ 0.04 MaNGA galaxies. We find evidence for outflows in 322 galaxies ($12{{\ \rm per\ cent}}$ of the analysed line-emitting sample), 185 of which show evidence for hosting an active galactic nucleus (AGN). Most outflows are centrally concentrated with a spatial extent that scales sublinearly with Re. The incidence of outflows is enhanced at higher masses, central surface densities, and deeper gravitational potentials, as well as at higher star formation rate (SFR) and AGN luminosity. We quantify strong correlations between mass outflow rates and the mechanical drivers of the outflow of the form $\dot{M}_{\rm out} \propto \rm SFR^{0.97}$ and $\dot{M}_{\rm out} \propto L_{\rm AGN}^{0.55}$. We derive a master scaling relation describing the mass outflow rate of ionized gas as a function of M⋆, SFR, Re, and LAGN. Most of the observed winds are anticipated to act as galactic fountains, with the fraction of galaxies with escaping winds increasing with decreasing potential well depth. We further investigate the physical properties of the outflowing gas finding evidence for enhanced attenuation in the outflow, possibly due to metal-enriched winds, and higher excitation compared to the gas in the galactic disc. Given that the majority of previous studies have focused on more extreme systems with higher SFRs and/or more luminous AGN, our study provides a unique view of the non-gravitational gaseous motions within ‘typical’ galaxies in the low-redshift Universe, where low-luminosity AGN and star formation contribute jointly to the observed outflow phenomenology.

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Rozprawy doktorskie na temat "Galactic Outflow"

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McGraw, Sean Michael. "Outflow and Accretion Physics in Active Galactic Nuclei". Ohio University / OhioLINK, 2016. http://rave.ohiolink.edu/etdc/view?acc_num=ohiou1469701247.

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Edmonds, Bartlett D. "On the Distances and Energetics of AGN Outflows". Diss., Virginia Tech, 2013. http://hdl.handle.net/10919/23767.

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Active galactic nuclei (AGN) ubiquitously show outflows. It is now widely recognized that these outflows are key components in the evolution of super-massive black holes and their host galaxies. As important as these outflows are, we still lack sufficient understanding of their structure and energetics. The majority of the work presented in this thesis involved photoionization modeling of AGN outflows along with analysis of density diagnostics in order to determine the distances and energetics of observed outflows. The main findings of these analyses are that 1) outflows are often at distances of hundreds to thousands of parsecs from the central supermassive black hole and 2) quasars outflows can be sufficiently powerful to provide feedback in galactic evolution scenarios. We also find in some cases that the recombination timescales of metal ions are long compared with the flux variability timescales. The large distances we find provide a challenge to current outflow models. For example, these outflows cannot be connected with an accretion disk surrounding the supermassive black hole as assumed in some models. Furthermore, the outflows may be out of equilibrium as we find in Mrk 509. In this case, a thorough understanding of time-dependent photoionization effects is necessary. In this thesis, I include early steps toward understanding time-dependent photoionization as well as ionization studies of accretion disk winds. The main results of these theoretical studies is that 1) the appearance of multiple ionization components in an outflow can be an artifact of the incorrect assumption that the outflow is in ionization equilibrium and 2) the shielding gas required in accretion-disk-wind models should have a clear signature in UV spectra, but none has been observed to date.
Ph. D.

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Moss, Vanessa. "The Galactic ecosystem: Outflow and infall in the halo of the Milky Way". Thesis, The University of Sydney, 2014. http://hdl.handle.net/2123/13488.

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The evolution, dynamics and eventual fate of galaxies is largely determined by access to and distribution of their primary fuel: atomic neutral hydrogen. Neutral hydrogen is not only pervasive in the disk of galaxies such as the Milky Way, but can also be found in the hot halo surrounding galaxies. The signatures of hydrogen detected in galactic haloes are caused by three key processes: outflow, due to energetic events associated with the galactic disk; infall, due to interactions with other nearby galaxies or the intergalactic medium; and circulation within the galactic ecosystem. In this thesis, a nearby Galactic supershell GSH 006-15+7 is studied, in order to understand how supershells are able to circulate cold gas between the disk and halo. By analysing HI self-absorption in the shell wall, the spin temperature of the gas is constrained to be cold and dense. Based on the morphology of the supershell and its estimated distance, GSH 006-15+7 has a likely origin in the Sagittarius OB 1 association of young stars. There is also evidence that the shell is transitioning into a chimney structure based on fragmentation at high Galactic latitudes, with an associated ionised hydrogen feature indicating a potential position of break-out into the Milky Way halo. This result is supported by findings in optical emission lines of high energy activity. Anomalous velocity gas deviates from that expected of Galactic rotation, and as such pinpoints hydrogen that is part of the cycle of outflow, infall and circulation. The Galactic All Sky Survey (GASS) of southern-sky neutral hydrogen is used to catalogue anomalous velocity gas in the halo of the Milky Way. Both classical high-velocity clouds and anomalous velocity clouds are included in the catalogue. With their lower velocities, anomalous velocity clouds are intrinsically closer to Galactic rotation and hence can be expected to probe the bridge between the Galactic disk and the halo. The GASS catalogue features unprecedented combination of high sensitivity with high angular and spectral resolution in the southern sky, and will be useful for studies of anomalous velocity gas on various scales. Several GASS clouds are followed up, some of known origin, at high angular resolution with the Australia Telescope Compact Array in order to determine the relative influences of origin and environment in clouds showing evidence of interaction. By combining the population of GASS high-velocity clouds with a very sensitive survey of neutral hydrogen in the halo, a Milky Way halo hidden from typical surveys of neutral hydrogen due to sensitivity limits is revealed, where the brightest neutral hydrogen merges with a diffuse prevalent medium that is likely to contribute just as much gas content as the bright high-velocity clouds. These results are consistent with findings in other wavelengths indicating the presence of more hydrogen in the halo than detected in the high-velocity cloud population. If the detected diffuse gas follows predicted supernova-driven models of cooling, then these two populations of neutral hydrogen combined can potentially account for the entire Galactic star formation rate. Overall, the studies in this thesis have revealed an active and dynamic Galaxy that maintains strong connections between its disk and the surrounding halo environment, in which neutral hydrogen remains a pivotal and powerful key to unlocking its evolutionary past and star-forming future.

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Ballone, Alessandro [Verfasser], i Andreas [Akademischer Betreuer] Burkert. "Hydrodynamical simulations of the Galactic Center cloud G2 as an outflow / Alessandro Ballone ; Betreuer: Andreas Burkert". München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2016. http://d-nb.info/1148276564/34.

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Xu, Xinfeng. "How Do Quasars Impact Their Host Galaxies? From the Studies of Quasar Outflows in Absorption and Emission". Diss., Virginia Tech, 2020. http://hdl.handle.net/10919/98572.

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``Quasar-mode feedback'' occurs when momentum and energy from the environment of accreting supermassive black hole couple to the host galaxy. One mechanism for such a coupling is by high-velocity (up to $sim$ 0.2c) quasar-driven ionized outflows, appearing as blue-shifted absorption and emission lines in quasar spectra. Given enough energy and momentum, these outflows are capable of affecting the evolution of their host galaxies. This dissertation presents the studies of emission and absorption quasar outflows from different perspectives. (1). By conducting large broad absorption line (BAL) quasar surveys in both Sloan Digital Sky Survey and Very Large Telescopes (VLT), we determined various physics properties of quasar absorption outflows, e.g., the electron number density (ne), the distance of outflows to the central quasar ($R$), and the kinetic energy carried by the outflow ($dot{E}_{k}$). We demonstrated that half of the typical BAL outflows are situated at $R$ $>$ 100 pc, i.e., having the potential to affect the host galaxies. (2). Our group carried out a Hubble Space Telescope program (PI: Arav) for studying the outflows in the Extreme-UV, collaborating with Dr. Gerard Kriss from Space Telescope Science Institute (STScI). We developed a novel method to fit the multitude of quasar absorption troughs efficiently and accurately. We have identified the most energetic quasar-driven outflows on record and discovered the largest acceleration and velocity-shift for a quasar absorption outflow. (3). By using the VLT data, Xu led the project to study the relationships between BAL outflows and emission line outflows. We found possible connections between these two types of quasar outflows, e.g., the luminosity of the [oiii] ly 5007 emission profile decreases with increasing ne derived from the BAL outflow in the same quasar. These findings are consistent with BAL and emission outflows being different manifestations of the same wind, and the observed relationships are likely a reflection of the outflow density distribution.
Doctor of Philosophy
Super massive black holes (SMBHs) are believed to exist in the center of almost all massive galaxies, where the brightest accreting ones are named ``quasars''. ``Quasar-mode feedback'' occurs when momentum and energy from the environment of accreting SMBHs couple to the host galaxy. One mechanism for such a coupling is by high-velocity (up to $sim$ 0.2c) quasar-driven ionized outflows, appearing as blue-shifted absorption and emission lines in quasar spectra. Given enough energy and momentum, these outflows are capable of affecting the evolution of their host galaxies. Such quasar outflows are invoked to explain a variety of observations, e.g., the chemical enrichment of the intergalactic medium (IGM), the shape of the observed quasar luminosity function, and the self-regulation of the growth of the SMBHs. In this dissertation, I focus on studying the emission and absorption outflows observed in quasars spectra, collected with the largest telescopes and most powerful instruments in the world. (1). By conducting large broad absorption line (BAL) quasar surveys in both Sloan Digital Sky Survey and Very Large Telescopes (VLT), we determined various physics properties of quasar absorption outflows, e.g., the electron number density (ne), the distance of outflows to the central quasar ($R$), and the kinetic energy carried by the outflow ($dot{E}_{k}$). We demonstrated that half of the typical BAL outflows are situated at $R$ $>$ 100 pc, i.e., having the potential to affect the host galaxies. (2). Our group carried out a Hubble Space Telescope program (PI: Arav) for studying the outflows in the Extreme-UV, collaborating with Dr. Gerard Kriss from Space Telescope Science Institute (STScI). We developed a novel method to fit the multitude of quasar absorption troughs efficiently and accurately. We have identified the most energetic quasar-driven outflows on record and discovered the largest acceleration and velocity-shift for a quasar absorption outflow. (3). By using the VLT data, Xu led the project to study the relationships between BAL outflows and emission line outflows. We found possible connections between these two types of quasar outflows, e.g., the luminosity of the [oiii] ly 5007 emission profile decreases with increasing ne derived from the BAL outflow in the same quasar. These findings are consistent with BAL and emission outflows being different manifestations of the same wind, and the observed relationships are likely a reflection of the outflow density distribution.

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Jeffrey, Robert. "The remarkable outflows from the galactic microquasar SS433". Thesis, University of Oxford, 2016. https://ora.ox.ac.uk/objects/uuid:b9f5657b-a122-464f-8c55-db349ba74c4c.

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In this thesis, I present 4 new, high-resolution observations of the Galactic microquasar SS 433, obtained from the Very Long Baseline Array (VLBA). I show that we can resolve the same ejecta in successive observations separated by ~ 35 d. I will demonstrate a method to uniquely determine launch vectors of the jet bolides, and I use this unprecedented baseline in time to show that the expansion rate of these bolides may reach 0.03c. I also present the first scientific results from the study of the radio jets in a unique set of historic observations of SS 433: the 39 images that comprise the 2003 VLBA movie of Mioduszewski et al. (2004). This unmatched time sampling allows us to see daily changes in the dynamics of SS 433's jets. I present evidence that these observations caught SS 433 as it transitioned from quiescence into a flare, and I show that this manifests itself as an increase in both the jet launch speed and the brightness of the jet bolides. Using these data, I examine the evolution of the particle energies, densities and magnetic fields within the bolides. We see that the estimates of the mass-loss rates via the jets cannot be reconciled with the those inferred from X-ray or optical data, if we posit equipartition of energy in synchrotron emitting plasma. The time resolution of the 2003 data allows us to observe the flux evolution of the jet bolides, and I show that the bolides undergo a power law decay as t^â2.8. Lastly, I examine X-ray monitoring data from the Swift/BAT satellite and the MAXI All-Sky- Monitor. From these lightcurves, I examine the geometry of the X-ray emission from close to the compact object itself, and I discuss SS 433's place within the current paradigm of accretion in microquasars. Throughout, we will see that it is the accessible time scales of the SS 433 phenomenon that allow us to learn about its exciting, complex physics.

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Cirasuolo, Michele. "AGN outflows and galaxy formation". Doctoral thesis, SISSA, 2004. http://hdl.handle.net/20.500.11767/4168.

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Nakashima, Shinya. "X-RAY STUDY ON PLASMA OUTFLOWS FROM THE GALACTIC CENTER". 京都大学 (Kyoto University), 2014. http://hdl.handle.net/2433/188484.

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Mehdipour, M. "Ionised outflows and multi-wavelength variability of Active Galactic Nuclei". Thesis, University College London (University of London), 2012. http://discovery.ucl.ac.uk/1379538/.

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This thesis presents a study of ionised outflows and multi-wavelength variability of Active Galactic Nuclei (AGN) focusing on three Seyfert-type objects: NGC 3516, Mrk 509 and ESO 113-G010. For this work I have made use of mostly XMM-Newton data, i.e. high-resolution X-ray spectra from the Reflection Grating Spectrometer (RGS) for exploring the ionised outflows, and simultaneous optical/UV/X-ray data from the Optical Monitor (OM) and the European Photon Imaging Camera (EPIC) instruments to study the intrinsic emission and variability. I have investigated the structure and geometry of the partial-covering multi-phase ionised absorber of NGC 3516. I demonstrate that the X-ray variability, originally attributed to occultation by a cloud in an accretion disc wind passing in front of the source, is rather the result of changes in the intrinsic emission of the source. From a 100-day multi-wavelength campaign on Mrk 509, I find that the character of its variability, strictly correlated in the UV and soft X-ray bands, indicates that the soft X-ray excess emission is produced by Compton reprocessing of the UV disc emission in a warm corona encasing the inner disc. I have also studied the nuclear obscuration and the role of dust in the warm absorber of ESO 113-G010. I show that the cause of significant optical/UV reddening, despite the lack of X-ray absorption from neutral gas, is most likely to be dust embedded in a weakly-ionised phase of an absorber which is conspicuous in the high-resolution X-ray spectrum of this object. I have explored the uncertainties in the irradiating spectral energy distribution due to the nuclear obscuration of the source and the effects these have on the survival of the dust, on the thermal stability of the warm absorber phases and the ionisation balance calculations required for photoionisation modelling. From my case-studies of these three objects emerges a more detailed picture of the ionised outflows phenomenon and of the environment in the vicinity of the nuclear supermassive black holes in AGN.

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Fields, Dale L. "Absorption-line measurements of AGN outflows". Columbus, Ohio : Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1155913695.

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Książki na temat "Galactic Outflow"

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1957-, Crenshaw Daniel Michael, Kraemer Steven B i George Ian M. 1963-, red. Mass outflow in active galactic nuclei: New perspectives : proceedings of a workshop held at the Catholic University of America, Washington, D.C., USA, 8-10 March 2001. San Francisco, Calif: Astronomical Society of the Pacific, 2002.

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Bianchi, Luciana, i Roberto Gilmozzi, red. Mass Outflows from Stars and Galactic Nuclei. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8.

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IAU Colloquium (163rd 1996 Port Douglas, Qld.). Accretion phenomena and related outflows: IAU Colloquium 163 : colloquium held in Port Douglas, Queensland, Australia, 15-19 July 1996. San Francisco, Calif: Astronomical Society of the Pacific, 1997.

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1954-, Bianchi Luciana, i Gilmozzi Roberto 1954-, red. Mass outflows from stars and galactic nuclei: Proceedings of the second Torino workshop, held in Torino, Italy, May 4-8, 1987. Dordrecht: Kluwer Academic Publishers, 1988.

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The role of the disk-halo interaction in galaxy evolution: Outflows vs infall : Espinho, Portugal, August 18-22, 2008. Les Ulis: EDP Sciences, 2012.

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Torino Workshop (2nd 1987 Torino, Italy). Mass outflows from stars and galactic nuclei: Proceedings of the second Torino Workshop, held in Torino, Italy, May 4-8, 1987. London: Kluwer, 1988.

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Crenshaw, D. M. Mass Outflow in Active Galactic Nuclei: New Perspectives: Proceedings of the Workshop on Mass Outflow in Active Galactic Nuclei, 2001: Washington, D. C. (Asp Conference Series Proceedings, Volume 255). Astronomical Society of the Pacific, 2002.

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Mass Outflows from Stars and Galactic Nuclei: Proceedings of the Second Torino Workshop, Held in Torino, Italy, May 4-8, 1987. Springer, 2011.

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Bianchi, Luciana, i Roberto Gilmozzi. Mass Outflows from Stars and Galactic Nuclei: Proceedings of the Second Torino Workshop, Held in Torino, Italy, May 4-8 1987. Springer, 2012.

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Bianchi, Luciana. Mass Outflows from Stars and Galactic Nuclei: "Proceedings of the Second Torino Workshop, Held in Torino, Italy, May 4-8, 1987". Springer, 2011.

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Części książek na temat "Galactic Outflow"

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Rees, Martin. "Mechanisms for Outflow in AGNs". W Mass Outflows from Stars and Galactic Nuclei, 163–76. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_13.

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Doazan, V., i R. N. Thomas. "Implications of Variable Mass-Outflow on Modeling". W Mass Outflows from Stars and Galactic Nuclei, 205–9. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_17.

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Tomisaka, Kohji. "Numerical Simulations of Galactic Outflow and Inflow Phenomena". W The Interstellar Disk-Halo Connection in Galaxies, 407–16. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3228-2_51.

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Noci, G. "Mass Outflow from the Sun —Observations and Diagnostics". W Mass Outflows from Stars and Galactic Nuclei, 11–23. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_2.

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Aglietta, M., G. Badino, G. Bologna, C. Castagnoli, A. Castellina, V. L. Dadykin, W. Fulgione i in. "Neutrino Outflow from Supernova 1987A Detected in the Mont Blanc Observatory". W Mass Outflows from Stars and Galactic Nuclei, 367–72. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_54.

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Muñoz-Tuñon, C., i John E. Beckman. "Observations of Outflow and its Consequences in Circum-Nuclear Zones of Spirals". W Mass Outflows from Stars and Galactic Nuclei, 391–95. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_59.

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Schilizzi, R. T. "Observational Evidence for Outflow in Active Galactic Nuclei and in X-Ray Binaries". W Mass Outflows from Stars and Galactic Nuclei, 151–62. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_12.

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Pismis, P., E. Moreno i A. Garcia-Barreto. "Collimated Bipolar Outflow and the Formation of Nuclear Spirals; Possible Role of Magnetic Fields". W Galactic and Intergalactic Magnetic Fields, 447–48. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0569-6_145.

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Phillips, J. P., i Glenn J. White. "J = 3−2 and J = 2−1 Co Mapping of High Velocity Outflow Sources". W Mass Outflows from Stars and Galactic Nuclei, 349–53. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_50.

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Cesaroni, Riccardo. "Outflow, Infall, and Rotation in High-Mass Star Forming Regions". W Dense Molecular Gas Around Protostars and in Galactic Nuclei, 5–17. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-3831-3_1.

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Streszczenia konferencji na temat "Galactic Outflow"

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Mertsch, Philipp, i Vahe Petrosian. "The Fermi Bubbles from Stochastic Acceleration by Turbulence in a Galactic Outflow". W 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.1108.

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Chen, Andrew, Sergio Colafrancesco i Nebiha Shafi. "Disentangling the gamma-ray emission of NGC 1068: The case for AGN-driven galactic outflow". W HIGH ENERGY GAMMA-RAY ASTRONOMY: 6th International Meeting on High Energy Gamma-Ray Astronomy. Author(s), 2017. http://dx.doi.org/10.1063/1.4968955.

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Bordas, Pol. "Relativistic Outflows From Compact Galactic Sources". W High Energy Phenomena in Relativistic Outflows VII. Trieste, Italy: Sissa Medialab, 2020. http://dx.doi.org/10.22323/1.354.0097.

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Pugmire, David, Paul Sutter, Paul Ricker, Hsiang-Yi (Karen) Yang i George Foreman. "Magnetic field outflows from active galactic nuclei". W the 2011 companion. New York, New York, USA: ACM Press, 2011. http://dx.doi.org/10.1145/2148600.2148668.

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Bomans, Dominik J. "Outflows and galactic winds of dwarf galaxies". W THE EVOLUTION OF STARBURSTS: The 331st Wilhelm and Else Heraeus Seminar. AIP, 2005. http://dx.doi.org/10.1063/1.2034972.

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Proga, Daniel, Ryuichi Kurosawa, Ivan Hubeny, James M. Stone, Keith MacGregor i Klaus Werner. "Radiation-Driven Outflows in Active Galactic Nuclei". W RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS: Proceedings of the International Conference in Honor of Dimitri Mihalas for His Lifetime Scientific Contributions on the Occasion of His 70th Birthday. AIP, 2009. http://dx.doi.org/10.1063/1.3250069.

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Holczer, Tomer, i Ehud Behar. "Ubiquitous thermal instability in active galactic nuclei outflows". W WAVES AND INSTABILITIES IN SPACE AND ASTROPHYSICAL PLASMAS. AIP, 2012. http://dx.doi.org/10.1063/1.3701363.

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Inoue, Susumu. "Cosmic ray acceleration and nonthermal emission from ultra-fast outflows in active galactic nuclei". W The 34th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.236.0925.

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Igarashi, Asuka, Masao Mori i Shin-ya Nitta. "Transonic galactic outflows and their influences to the chemical evolution of galaxies and intergalactic space". W ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2013: Proceedings of the 12th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG12). AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4874049.

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Yaqoob, Tahir. "Outflows, Accretion Disks & the IGM: High Resolution Chandra & XMM Spectroscopy of Active Galactic Nuclei". W X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: Theory, Experiment, and Observation. AIP, 2005. http://dx.doi.org/10.1063/1.1960947.

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