Continuous stellar mass-loss in<i>N</i>-body models of galaxies

Jungwiert, Bruno; Combes, F.; Palouš, J.

doi:10.1051/0004-6361:20010966

Cited by 81 publications

(99 citation statements)

References 20 publications

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“…We use the following fitting formula proposed by Jungwiert, Combes & Palouš (2001) to describe R(t):…”

Section: Appendix C: Time Dependent Stellar Mass Loss Modelmentioning

confidence: 99%

Formation of disc galaxies in preheated media: a preventative feedback model

Lu¹,

Mo²

2014

Monthly Notices of the Royal Astronomical Society

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We introduce a semi-analytic galaxy formation model implementing a self-consistent treatment for the hot halo gas configuration and the assembly of central disks. Using the model, we explore a preventative feedback model, in which the circum-halo medium is assumed to be preheated up to a certain entropy level by early starbursts or other processes, and compare it with an ejective feedback model, in which baryons are first accreted into dark matter halos and subsequently ejected out by feedback. The model demonstrates that when the medium is preheated to an entropy comparable to the halo virial entropy the baryon accretion can be largely reduced and delayed. In addition, the preheated medium can establish an extended low density gaseous halo when it accretes into the dark matter halos, and result in a specific angular momentum of the cooling gas large enough to form central disks as extended as those observed. Combined with simulated halo assembly histories, the preventative feedback model can reproduce remarkably well a number of observational scaling relations. These include the cold baryon (stellar plus cold gas) mass fraction-halo mass relations, star formation histories, disk size-stellar mass relation and its evolution, and the number density of low-mass galaxies as a function of redshift. In contrast, the conventional ejective feedback model fails to reproduce these observational trends. Using the model, we demonstrate that the properties of disk galaxies are closely tied to the thermal state of hot halo gas and even possibly the circum-halo medium, which suggests that observational data for the disk properties and circum-galactic hot/warm medium may jointly provide interesting constraints for galaxy formation models.

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“…We use the following fitting formula proposed by Jungwiert, Combes & Palouš (2001) to describe R(t):…”

Section: Appendix C: Time Dependent Stellar Mass Loss Modelmentioning

confidence: 99%

Formation of disc galaxies in preheated media: a preventative feedback model

Lu¹,

Mo²

2014

Monthly Notices of the Royal Astronomical Society

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“…di Matteo et al 2007), before sufficient stellar mass is accumulated and a star particle can be created. Continuous mass loss is also considered, with about 40% of the stellar mass loss by young massive stars after 5 Gyr (Jungwiert et al 2001). The energy reinjected by supernovae into the interstellar medium is assumed to be a kinematic feedback on neighboring gas particles: each neighbor of an SPH particle having formed δm of stars is given a radial kick in velocity away from the supernova formed.…”

Section: Techniquementioning

confidence: 99%

Dust and gas power spectrum in M 33 (HERM33ES)

Combes

Boquien

Krämer

et al. 2012

A&A

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Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from −1.5 to −4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M /yr, with 10% supernovae energy coupled to the gas kinematics.

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“…We implement continuous, time dependent stellar mass recycling following Jungwiert et al (2001). They give the …”

Section: A Model For Dust Formationmentioning

confidence: 99%

“…The rate at which stellar mass is recycled to the ISM is given as a convolution of the SFR with the time derivative of the fractional mass recycled. Jungwiert et al (2001) parameterize the fractional mass recycled from a single, instantaneous burst stellar population as a function of time by…”

Section: Smrr Asṁmentioning

confidence: 99%

The slow flow model of dust efflux in local star-forming galaxies

Zahid

Torrey

Kudritzki

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We develop a dust efflux model of radiation pressure acting on dust grains which successfully reproduces the relation between stellar mass, dust opacity and star formation rate observed in local star-forming galaxies. The dust content of local star-forming galaxies is set by the competition between the physical processes of dust production and dust loss in our model. The dust loss rate is proportional to the dust opacity and star formation rate. Observations of the relation between stellar mass and star formation rate at several epochs imply that the majority of local star-forming galaxies are best characterized as having continuous star formation histories. Dust loss is a consequence of sustained interaction of dust with the radiation field generated by continuous star formation. Dust efflux driven by radiation pressure rather than dust destruction offers a more consistent physical interpretation of the dust loss mechanism. By comparing our model results with the observed relation between stellar mass, dust extinction and star formation rate in local star-forming galaxies we are able to constrain the timescale and magnitude of dust loss. The timescale of dust loss is long and therefore dust is effluxed in a "Slow Flow". Dust loss is modest in low mass galaxies but massive galaxies may lose up to 70 ∼ 80% of their dust over their lifetime. Our Slow Flow model shows that mass loss driven by dust opacity and star formation may be an important physical process for understanding normal star-forming galaxy evolution.

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Continuous stellar mass-loss inN-body models of galaxies

Cited by 81 publications

References 20 publications

Formation of disc galaxies in preheated media: a preventative feedback model

Formation of disc galaxies in preheated media: a preventative feedback model

Dust and gas power spectrum in M 33 (HERM33ES)

The slow flow model of dust efflux in local star-forming galaxies

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