Please use this identifier to cite or link to this item:
http://hdl.handle.net/2289/6674Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Yadav, Naveen | - |
| dc.contributor.author | Mukherjee, Dipanjan | - |
| dc.contributor.author | Sharma, Prateek | - |
| dc.contributor.author | Nath, Biman B. | - |
| dc.date.accessioned | 2017-07-10T13:56:21Z | - |
| dc.date.available | 2017-07-10T13:56:21Z | - |
| dc.date.issued | 2017-02 | - |
| dc.identifier.citation | Monthly Notices of the Royal Astronomical Society Letters , 2016, Vol. 465, p1720-1740 | en_US |
| dc.identifier.issn | 0035-8711 | - |
| dc.identifier.issn | 1365-2966 (Online) | - |
| dc.identifier.uri | http://hdl.handle.net/2289/6674 | - |
| dc.description | Open Access | en_US |
| dc.description.abstract | We explore the formation of superbubbles through energy deposition by multiple supernovae (SNe) in a uniform medium. We use the total energy conserving, 3D hydrodynamic simulations to study how SNe correlated in space and time create superbubbles. While isolated SNe fizzle out completely by ∼1 Myr due to radiative losses, for a realistic cluster size it is likely that subsequent SNe go off within the hot/dilute bubble and sustain the shock till the cluster lifetime. For realistic cluster sizes, we find that the bubble remains overpressured only if, for a given ng0, NOB is sufficiently large. While most of the input energy is still lost radiatively, superbubbles can retain up to ∼5–10 per cent of the input energy in the form of kinetic+thermal energy till 10 Myr for interstellar medium density ng0 ≈ 1 cm−3. We find that the mechanical efficiency decreases for higher densities ( ηmech∝n−2/3g0 ηmech∝ng0−2/3 ng0, NOB is sufficiently large. While most of the input energy is still lost radiatively, superbubbles can retain up to ∼5–10 per cent of the input energy in the form of kinetic+thermal energy till 10 Myr for interstellar medium density ng0 ≈ 1 cm−3. We find that the mechanical efficiency decreases for higher densities ( ηmech∝n−2/3g0 ηmech∝ng0−2/3 ). We compare the radii and velocities of simulated supershells with observations and the classical adiabatic model. Our simulations show that the superbubbles retain only ≲ 10 per cent of the injected energy, thereby explaining the observed smaller size and slower expansion of supershells. We also confirm that a sufficiently large (≳ 104) number of SNe are required to go off in order to create a steady wind with a stable termination shock within the superbubble. We show that the mechanical efficiency increases with increasing resolution, and that explicit diffusion is required to obtain converged results. | en_US |
| dc.language.iso | en | en_US |
| dc.publisher | Oxford University Press for the Royal Astronomical Society | en_US |
| dc.relation.uri | http://adsabs.harvard.edu/abs/2016MNRAS.tmp.1524Y | en_US |
| dc.relation.uri | http://arxiv.org/abs/1603.00815 | en_US |
| dc.relation.uri | http://dx.doi.org/10.1093/mnras/stw2522 | en_US |
| dc.rights | 2016 The authors & the Royal Astronomical Society | en_US |
| dc.subject | hydrodynamics, methods | en_US |
| dc.subject | numerical, ISM | en_US |
| dc.subject | bubbles | en_US |
| dc.title | How multiple supernovae overlap to form superbubbles | en_US |
| dc.type | Article | en_US |
| Appears in Collections: | Research Papers (A&A) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| 2017_MNRAS_465_1720.pdf | Open Access | 5.55 MB | Adobe PDF | View/Open |
Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.