A connection between star formation activity and cosmic rays in the starburst galaxy M82
V. A. AcciariE. AliuT. ArlenT. AuneM. A. BautistaM. BeilickeW. BenbowD. BoltuchS. M. BradburyJ. H. BuckleyV. BugaevK. ByrumA. CannonÖ. ÇelikA. CesariniY. C. ChowL. CiupikP. CoganP. ColinWei CuiR. DickherberC. DukeS. FeganJ. P. FinleyG. FinneganP. FortinL. FortsonA. FurnissN. GalanteD. GallK. GibbsG. H. GillandersS. GodambeJ. GrubeR. GuenetteG. GyukD. HannaJ. HolderD. HoranC. M. HuiT. B. HumenskyA. ImranP. KaaretN. KarlssonM. KertzmanD. KiedaJ. KildeaA. KonopelkoH. KrawczynskiF. KrennrichM. J. LangS. LeBohecG. MaierS. McArthurA. McCannM. McCutcheonJ. MillisP. MoriartyR. MukherjeeT. NagaiR. A. OngA. N. OtteD. PandelJ. S. PerkinsFilip PizloM. PohlJ. QuinnK. RaganL. C. ReyesP. T. ReynoldsE. RoacheH. J. RoseM. SchroedterG. H. SembroskiA. W. SmithD. SteeleS. P. SwordyM. TheilingS. ThibadeauA. VarlottaV. V. VassilievS. VincentR. G. WagnerS. P. WakelyJ. E. WardT. C. WeekesA. J. WeinsteinT. WeisgarberD. A. WilliamsStephanie WisselM. WoodB. Zitzer
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Author(s): Feindt, U; Kerschhaggl, M; Kowalski, M; Aldering, G; Antilogus, P; Aragon, C; Bailey, S; Baltay, C; Bongard, S; Buton, C; Canto, A; Cellier-Holzem, F; Childress, M; Chotard, N; Copin, Y; Fakhouri, HK; Gangler, E; Guy, J; Kim, A; Nugent, P; Nordin, J; Paech, K; Pain, R; Pecontal, E; Pereira, R; Perlmutter, S; Rabinowitz, D; Rigault, M; Runge, K; Saunders, C; Scalzo, R; Smadja, G; Tao, C; Thomas, RC; Weaver, BA; Wu, C
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We observe the heating of interstellar material in young supernova remnants (SNR). In addition, when analyzing the soft X-ray background we find evidence for large isolated regions of apparently hot, low density material. These, we infer, may have been heated by supernovae. One such region seems to surround the Sun. This has been modeled as a supernova remnant viewed from within. The most reasonable parameters are ambient density n o ~ 0.004 cm −3 , radius of about 100 pc, age just over 10 5 years (Cox and Anderson 1982).
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Massive stars can significantly modify the surrounding medium during their lifetime. When the stars explode as supernovae, the resulting shock wave expands within this modified medium and not within the interstellar medium. We explore the evolution of the medium around massive stars, and the expansion of the shock wave within this medium. We then apply these results to understanding the expansion of the shock wave in the ambient medium surrounding SN 1987A, and the evolution of the radio and X-ray emission in this case.
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Supernovae are very luminous events, on the scale of entire galaxies, and deposit mass and large amounts of energy in to the surrounding interstellar medium. In this work the effect of a supernova on the surrounding medium is studied. The evolution of the remnant is assumed to be spherical symmetric. The hydrodynamic evolution of the system is simulated for different density distributions of the ambient medium and compared to analytically solutions where they exists. Some background theory about stellar evolution and supernovae is given. Since strong shocks from supernovae is interesting in the context of cosmic ray acceleration some theory about cosmic is included. The framework for simulating the hydrodynamic equations governing the system is based on the work done by W.Benz.
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Supernova (SN) explosions play an important role in the development of galactic structures. The energy and momentum imparted on the interstellar medium (ISM) in so-called "supernova feedback" drives turbulence, heats the gas, enriches it with heavy elements, can lead to the formation of new stars or even suppress star formation by disrupting stellar nurseries. In the numerical simulation at the sub-galactic level, not including the energy and momentum of supernovas in the physical description of the problem can also lead to several problems that might partially be resolved by including a description of supernovas. In this thesis such an implementation is attempted for the combined numerical hydrodynamics and N-body simulation software Arepo (Springel, 2010) for the high density gas in the ISM only. This allows supernova driven turbulence in boxes of 400pc cubed to be studied. In a stochastic process a large amount of thermal energy is imparted on a number of neighbouring cells, mimicking the effect of a supernova explosions. We test this approach by modelling the explosion of a single supernova in a uniform density medium and comparing the evolution of the resulting supernova remnant to the theoretically-predicted behaviour. We also run a simulation with our feedback code and a fixed supernova rate derived from the Kennicutt-Schmidt relation (Kennicutt, 1998) for a duration of about 20 Myrs. We describe our method in detail in this text and discuss the properties of our implementation. vii
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Abstract Supernovae are the most energetic stellar events and influence the interstellar medium by their gasdynamics and energetics. By this, both also affect the star formation positively and negatively. In this paper, we review the development of the complexity of investigations aiming at understanding the interchange between supernovae and their released hot gas with the star-forming molecular clouds. Commencing from analytical studies the paper advances to numerical models of supernova feedback from superbubble scales to galaxy structure. We also discuss parametrizations of star-formation and supernova-energy transfer efficiencies. Since evolutionary models from the interstellar medium to galaxies are numerous and apply multiple recipes of these parameters, only a representative selection of studies can be discussed here.
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Supernova remnants (SNRs) are remarkable astronomical objects which are a diffuse, expanding nebula of gas that is a direct result of a star's explosive death, resulting in a supernova explosion. SNRs play a vital role in the scattering of tough elements which are made in the supernova explosion into the interstellar medium and provide much amount of energy that heats the ISM, as well as SNRs, are responsible for enormous differences in physical process and properties. In the present work, we study the physical properties, performance, and behavior of dynamical growth of several SNR type Ia and type II specifically after an explosion of a supernova, and explore how the density of the interstellar environment influence the physical properties and eternity of each SNRs. To achieve such goals, we have utilized the method known as Counting Pixels Method, which has been applied to the SNRs images as well as a new pattern has been suggested to calculate some of the physical properties such as the expansion velocity and the radius of the chosen remnants, which based on the age of SNRs and the density of the surrounding medium. The outcomes of the study depicted that each chosen SNRs type Ia and II likewise in performance and behavior after a long period of explosion nevertheless, they are displaced either upwards or downwards based on the interstellar density. However, we noted that SNRs are exploded in the lower density environment and expanded without restriction to make a regular shape. We have concluded that further study is required particularly on the physical properties of SNRs when inserted into the radiative phase.
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Abstract Supernovae are the most energetic stellar events and influence the interstellar medium by their gasdynamics and energetics. By this, both also affect the star formation positively and negatively. In this paper, we review the complexity of investigations aiming at understanding the interchange between supernova explosions with the star-forming molecular clouds. Commencing from analytical studies the paper advances to numerical models of supernova feedback from superbubble scales to galaxy structure. We also discuss parametrizations of star-formation and supernova-energy transfer efficiencies. Since evolutionary models from the interstellar medium to galaxies are numerous and are applying multiple recipes of these parameters, only a representative selection of studies can be discussed here.
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