2014
DOI: 10.1093/mnras/stu1414
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Angular momentum transport and evolution of lopsided galaxies

Abstract: The surface brightness distribution in the majority of stellar galactic discs falls off exponentially. Often what lies beyond such a stellar disc is the neutral hydrogen gas whose distribution also follows a nearly exponential profile at least for a number of nearby disc galaxies. Both the stars and gas are commonly known to host lopsided asymmetry especially in the outer parts of a galaxy. The role of such asymmetry in the dynamical evolution of a galaxy has not been explored so far.Following Lindblad's origi… Show more

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Cited by 18 publications
(16 citation statements)
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“…In the present paper we focus on "lop-sided" (off-centre, or seiche) modes, because these have the lowest damping rates of the modes which Weinberg discovered. Such modes have long been of interest in flattened systems, especially spiral galaxies, but also in the dynamics of dark matter halos (Saha et al 2009;De Rijcke et al 2011;Mirtadjieva et al 2011;Jütte et al 2013;Zaritsky et al 2013;Yozin & Bekki 2014;Saha & Jog 2014;Prasad & Jog 2017;Wu et al 2017;Vulcani et al 2018).…”
Section: Introductionmentioning
confidence: 99%
“…In the present paper we focus on "lop-sided" (off-centre, or seiche) modes, because these have the lowest damping rates of the modes which Weinberg discovered. Such modes have long been of interest in flattened systems, especially spiral galaxies, but also in the dynamics of dark matter halos (Saha et al 2009;De Rijcke et al 2011;Mirtadjieva et al 2011;Jütte et al 2013;Zaritsky et al 2013;Yozin & Bekki 2014;Saha & Jog 2014;Prasad & Jog 2017;Wu et al 2017;Vulcani et al 2018).…”
Section: Introductionmentioning
confidence: 99%
“…Could it be that the classical bulge grew at the cost of disc fading? If this is indeed true, it might be an indication of the secular process in action -where disc materials help developing central concentration via redistribution of angular momentum which is known to occur due to non-axisymmetries present in the disc (Kormendy & Kennicutt 2004;Saha & Jog 2014). Our analysis suggests that a joint role played by inwardmigration of star-forming clumps, minor mergers and secular processes is behind the overall growth of bulges since z ∼ 1.…”
Section: Summary and Discussionmentioning
confidence: 70%
“…This is a drastically different scenario when compared to the two-fluid gas-rich infinitesimally-thin system. Spiral arms are known to transport angular momentum (Lynden-Bell & Kalnajs 1972;Saha & Jog 2014) and are one of the main drivers for the secular evolution of galaxies. Since the inclusion of finite thickness of disk can lead to the suppression of formation of strong, small-scale spiral arms (as shown here), therefore, finite thickness of a disk could have a non-trivial effect of delaying the long-term evolution of disk galaxies.…”
Section: Resultsmentioning
confidence: 99%