Primordial magnetic fields in population III star formation: a magnetized resolution study
Population III (Pop III) stars form in groups due to the fragmentation of primordial gas. While uniform magnetic fields have been shown to support against fragmentation in present-day star formation, it is unclear whether realistic k3/2 primordial fields can have the same effect. We bypass the issue...
Gespeichert in:
| Hauptverfasser: | , , , , |
|---|---|
| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2022 August 8
|
| In: |
Monthly notices of the Royal Astronomical Society
Year: 2022, Jahrgang: 516, Heft: 2, Pages: 2223-2234 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stac2327 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stac2327
|
| Verfasserangaben: | Lewis R. Prole, Paul C. Clark, Ralf S. Klessen, Simon C.O. Glover and Rüdiger Pakmor |
MARC
| LEADER | 00000caa a2200000 c 4500 | ||
|---|---|---|---|
| 001 | 1819066274 | ||
| 003 | DE-627 | ||
| 005 | 20240326080217.0 | ||
| 007 | cr uuu---uuuuu | ||
| 008 | 221018s2022 xx |||||o 00| ||eng c | ||
| 024 | 7 | |a 10.1093/mnras/stac2327 |2 doi | |
| 035 | |a (DE-627)1819066274 | ||
| 035 | |a (DE-599)KXP1819066274 | ||
| 035 | |a (OCoLC)1361693892 | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rda | ||
| 041 | |a eng | ||
| 084 | |a 29 |2 sdnb | ||
| 100 | 1 | |a Prole, Lewis R. |e VerfasserIn |0 (DE-588)1255776943 |0 (DE-627)1799932311 |4 aut | |
| 245 | 1 | 0 | |a Primordial magnetic fields in population III star formation |b a magnetized resolution study |c Lewis R. Prole, Paul C. Clark, Ralf S. Klessen, Simon C.O. Glover and Rüdiger Pakmor |
| 264 | 1 | |c 2022 August 8 | |
| 300 | |a 12 | ||
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a Computermedien |b c |2 rdamedia | ||
| 338 | |a Online-Ressource |b cr |2 rdacarrier | ||
| 500 | |a Gesehen am 18.10.2022 | ||
| 520 | |a Population III (Pop III) stars form in groups due to the fragmentation of primordial gas. While uniform magnetic fields have been shown to support against fragmentation in present-day star formation, it is unclear whether realistic k3/2 primordial fields can have the same effect. We bypass the issues associated with simulating the turbulent dynamo by introducing a saturated magnetic field at equipartition with the velocity field when the central densities reach 10−13 g cm−3. We test a range of sink particle creation densities from 10−10 to 10−8 g cm−3. Within the range tested, the fields did not suppress fragmentation of the gas and hence could not prevent the degree of fragmentation from increasing with increased resolution. The number of sink particles formed and total mass in sink particles was unaffected by the magnetic field across all seed fields and resolutions. The magnetic pressure remained sub-dominant to the gas pressure except in the highest density regions of the simulation box, where it became equal to but never exceeded gas pressure. Our results suggest that the inclusion of magnetic fields in numerical simulations of Pop III star formation is largely unimportant. | ||
| 700 | 1 | |a Clark, Paul C. |d 1979- |e VerfasserIn |0 (DE-588)1043520252 |0 (DE-627)770635490 |0 (DE-576)394879236 |4 aut | |
| 700 | 1 | |a Klessen, Ralf S. |d 1968- |e VerfasserIn |0 (DE-588)120533820 |0 (DE-627)392381532 |0 (DE-576)178685399 |4 aut | |
| 700 | 1 | |a Glover, Simon |e VerfasserIn |0 (DE-588)1043520449 |0 (DE-627)770635903 |0 (DE-576)394879252 |4 aut | |
| 700 | 1 | |a Pakmor, Rüdiger |d 1982- |e VerfasserIn |0 (DE-588)14360905X |0 (DE-627)647700670 |0 (DE-576)337951543 |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |a Royal Astronomical Society |t Monthly notices of the Royal Astronomical Society |d Oxford : Oxford Univ. Press, 1827 |g 516(2022), 2, Seite 2223-2234 |h Online-Ressource |w (DE-627)314059164 |w (DE-600)2016084-7 |w (DE-576)090955420 |x 1365-2966 |7 nnas |
| 773 | 1 | 8 | |g volume:516 |g year:2022 |g number:2 |g pages:2223-2234 |g extent:12 |a Primordial magnetic fields in population III star formation a magnetized resolution study |
| 856 | 4 | 0 | |u https://doi.org/10.1093/mnras/stac2327 |x Verlag |x Resolving-System |z lizenzpflichtig |3 Volltext |
| 951 | |a AR | ||
| 992 | |a 20221018 | ||
| 993 | |a Article | ||
| 994 | |a 2022 | ||
| 998 | |g 14360905X |a Pakmor, Rüdiger |m 14360905X:Pakmor, Rüdiger |d 130000 |d 130300 |e 130000PP14360905X |e 130300PP14360905X |k 0/130000/ |k 1/130000/130300/ |p 5 |y j | ||
| 998 | |g 1043520449 |a Glover, Simon |m 1043520449:Glover, Simon |d 700000 |d 714000 |d 714200 |d 700000 |d 728500 |e 700000PG1043520449 |e 714000PG1043520449 |e 714200PG1043520449 |e 700000PG1043520449 |e 728500PG1043520449 |k 0/700000/ |k 1/700000/714000/ |k 2/700000/714000/714200/ |k 0/700000/ |k 1/700000/728500/ |p 4 | ||
| 998 | |g 120533820 |a Klessen, Ralf S. |m 120533820:Klessen, Ralf S. |d 700000 |d 714000 |d 714200 |d 700000 |d 728500 |e 700000PK120533820 |e 714000PK120533820 |e 714200PK120533820 |e 700000PK120533820 |e 728500PK120533820 |k 0/700000/ |k 1/700000/714000/ |k 2/700000/714000/714200/ |k 0/700000/ |k 1/700000/728500/ |p 3 | ||
| 999 | |a KXP-PPN1819066274 |e 4198573247 | ||
| BIB | |a Y | ||
| SER | |a journal | ||
| JSO | |a {"name":{"displayForm":["Lewis R. Prole, Paul C. Clark, Ralf S. Klessen, Simon C.O. Glover and Rüdiger Pakmor"]},"language":["eng"],"person":[{"display":"Prole, Lewis R.","family":"Prole","role":"aut","given":"Lewis R.","roleDisplay":"VerfasserIn"},{"role":"aut","given":"Paul C.","family":"Clark","display":"Clark, Paul C.","roleDisplay":"VerfasserIn"},{"roleDisplay":"VerfasserIn","family":"Klessen","display":"Klessen, Ralf S.","role":"aut","given":"Ralf S."},{"roleDisplay":"VerfasserIn","given":"Simon","role":"aut","display":"Glover, Simon","family":"Glover"},{"family":"Pakmor","display":"Pakmor, Rüdiger","role":"aut","given":"Rüdiger","roleDisplay":"VerfasserIn"}],"origin":[{"dateIssuedDisp":"2022 August 8","dateIssuedKey":"2022"}],"recId":"1819066274","title":[{"title_sort":"Primordial magnetic fields in population III star formation","subtitle":"a magnetized resolution study","title":"Primordial magnetic fields in population III star formation"}],"relHost":[{"language":["eng"],"recId":"314059164","origin":[{"publisherPlace":"Oxford ; Oxford [u.a.] ; Oxford [u.a.]","dateIssuedDisp":"1827-","publisher":"Oxford Univ. Press ; Blackwell ; Wiley-Blackwell","dateIssuedKey":"1827"}],"disp":"Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society","title":[{"title_sort":"Monthly notices of the Royal Astronomical Society","title":"Monthly notices of the Royal Astronomical Society"}],"part":{"text":"516(2022), 2, Seite 2223-2234","year":"2022","extent":"12","volume":"516","pages":"2223-2234","issue":"2"},"physDesc":[{"extent":"Online-Ressource"}],"id":{"issn":["1365-2966"],"eki":["314059164"],"zdb":["2016084-7"],"doi":["10.1111/(ISSN)1365-2966"]},"note":["Gesehen am 15.01.2018"],"type":{"media":"Online-Ressource","bibl":"periodical"},"pubHistory":["1.1827 -"],"corporate":[{"roleDisplay":"VerfasserIn","role":"aut","display":"Royal Astronomical Society"}]}],"note":["Gesehen am 18.10.2022"],"id":{"eki":["1819066274"],"doi":["10.1093/mnras/stac2327"]},"physDesc":[{"extent":"12 S."}],"type":{"bibl":"article-journal","media":"Online-Ressource"}} | ||
| SRT | |a PROLELEWISPRIMORDIAL2022 | ||