![Page 1: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/1.jpg)
1
Evolution of rotating
magnetized starsDavid R. Aguilera-Dena, Universität Bonn
In collaboration with:Norbert langer, takashi Moriya & Abel Schootemeijer
+Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko Nakamura
![Page 2: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/2.jpg)
2
Before we begin: How do (massive) stars normally
evolve??
![Page 3: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/3.jpg)
3
⋆ Stars are in hydrostatic & thermal equilibrium
⋆ More massive stars evolve faster, roughly
⋆ More massive stars are also more luminous
⋆ They are also rare!
Main sequence massive stars
![Page 4: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/4.jpg)
4
⋆ Stars are in hydrostatic & thermal equilibrium
⋆ More massive stars evolve faster, roughly
⋆ More massive stars are also more luminous
⋆ They are also rare!
Main sequence massive stars
![Page 5: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/5.jpg)
5
⋆ Stars burn heavier metals until they form an iron core
⋆ Neutrino emission from thermal and nuclear processes becomes more important
⋆ Evolution is accelerated
⋆ Iron core formation leads to core collapse!
Late evolution of massive stars
![Page 6: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/6.jpg)
6
SNe
Not the whole story: The SN Zoo!
Type I Type II
Ia (thermonuclear) Ib Ic IIP IIL IIn IIb Type II SLSN
Type I SLSN
etc!
Ic-BL GRB-SN
etc!
Ultrastripped
![Page 7: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/7.jpg)
7
Progenitors: What we know so far...
Relative rates from volume-limited samples (Li et al. 2010, Shivvers et al. 2017)
![Page 8: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/8.jpg)
8
Type II Progenitors: the RSG problem
Masses of observed SN progenitors and KEPLER model ZAMS masses, Sukhbold & Adams 2019
![Page 9: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/9.jpg)
9
Type II Progenitors: the RSG problem
Kippenhahn diagrams of presupernova models from and their compactness, from Sukhbold et al. 2018
![Page 10: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/10.jpg)
10
Other uncertainties in massive star evolution
HR diagrams of evolutionary tracks with SMC metallicity, with different overshooting and semiconvection parameters, Schootemeijer et al. 2019
![Page 11: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/11.jpg)
11
Other uncertainties in massive star evolution
Observed and inferred distributions of massive binary periods, Sana et al. 2012
![Page 12: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/12.jpg)
12
Other uncertainties in massive star evolution
Circulation patterns in binary stars, Hastings et al. in prep.
![Page 13: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/13.jpg)
13
Other uncertainties in massive star evolution
HR diagram of a binary population in the LMC after 10 Myr, Bachelor thesis of S. Adscheid, see also the work by C. Wang
![Page 14: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/14.jpg)
14
Moving on to the very energetic explosions...
![Page 15: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/15.jpg)
15
Type I SLSNe
Example light curves from Smartt 2012
![Page 16: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/16.jpg)
16
⋆ Have no hydrogen or helium in their spectra (this probably means they have almost no H and He, see Hachinger et al. 2012)
⋆ They have very high energies
⋆ Their spectra show mostly O lines and are very hot
⋆ Found preferably in low metallicity environments (e.g. Lunnan et al. 2015)
Type I SLSNe
![Page 17: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/17.jpg)
17
⋆ Powered by a central magnetar (Kasen & Bildsten 2010, Nicholl et al. 2017)
⋆ Powered by interaction with the CSM (Chevalier 1982, Chevalier & Fransson 1994)
⋆ They’re actually PISNe! (see, e.g. Chatzopoulos et al. 2015)
⋆ Powered by fallback accretion (Moriya et al. 2018)
Type I SLSNe
![Page 18: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/18.jpg)
18
The magnetar model
Inferred properties of SLSNe in the magnetar model, from Nicholl et al. 2017
![Page 19: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/19.jpg)
19
⋆ They are related to massive stars and to Ic-BL SNe (Hjorth et al. 2003, Levan et al. 2016)
⋆ They form collimated relativistic jets (e.g. Piran 2004)
⋆ Their host galaxies are generally at low Z (Levan et al. 2016)
⋆ Most favored progenitor model is the collapsar model (Woosley 1993)
Gamma ray bursts (and their SNe)
![Page 20: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/20.jpg)
20
Fast rotation&
Low metallicity
![Page 21: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/21.jpg)
21
Not the first time it's been done
Similar to Yoon et al. 2006, Szécsi et al. 2015
![Page 22: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/22.jpg)
22
Not the first time it's been done
Rotational mixing has been enhanced by a factor 10, from Aguilera-Dena & Langer, in prep.
![Page 23: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/23.jpg)
23
Evolution with extreme rotation
⋆ Mixing leads to CHE
⋆ Lack of H/He shell leads to contraction
⋆ Contraction accelerates due to neutrinos
⋆
![Page 24: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/24.jpg)
24
Evolution with extreme rotation
⋆ Contraction leads to differential rotation (mostly small)
⋆ Angular momentum is transported to the surface (by magnetic fields)
⋆ Critical rotation very likely!
![Page 25: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/25.jpg)
25
Evolution with extreme rotation
![Page 26: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/26.jpg)
26
Evolution with extreme rotation
![Page 27: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/27.jpg)
27
Evolution with extreme rotation
⋆ Differential rotation leads to formation of magnetic fields
⋆ Magnetic fields can be strong enough to power SLSNe!
![Page 28: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/28.jpg)
28
Variety in magnetic fields!
![Page 29: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/29.jpg)
29
Evolution with extreme rotation
⋆ Expected observable features
- Interaction with dense CSM
- Fast rotating remnant
- Power from rotation being deposited into explosion
⋆ Enough angular momentum in the core to produce a GRB if black hole forms
![Page 30: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/30.jpg)
30
Evolution with extreme rotation
⋆ How to know if they form a magnetar (and a SLSN) or a black hole (and a long GRB)?
- Compactness parameter
- Core properties (mass gradient, core mass)
- Stellar structure
⋆ We need 2D/3D to see the impact of structure, rotation and magnetic fields!
![Page 31: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/31.jpg)
31
Evolution with extreme rotation
7, 8 and 9 Msun
![Page 32: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/32.jpg)
Evolution with extreme rotation
Comparison with the values obtained through the magnetar model by Nicholl et al. 2017
32
![Page 33: Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh ...blogs.exeter.ac.uk/supernova/files/2019/05/slides_david.pdf · Kei Kotake, Tomoya Takiwaki, Takashi Yoshida, Koh takahashi & Ko](https://reader036.vdocuments.pub/reader036/viewer/2022062610/61158d8f52447f7e9925d8ff/html5/thumbnails/33.jpg)
33
⋆ Massive star evolution is complicated! Many uncertainties go into characterizing the progenitors of the observed SN population
⋆ We discovered a new evolutionary channel where fast rotation and neutrino emission get together to form extreme conditions
⋆ It could lead to SLSNe or GRBs depending on explosion physics and late evolution, needs to be studied in 2D and 3D!
⋆ Core evolution has similarities to non-rotators, but explosions are different due to rotation and CSM
⋆ Important to consider rotation and magnetic fields in more detail since they appear in many extreme astrophysical situations
Conclusions