transport of angular momentum within stars · impact of post-ms angular momentum transport on...
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Transport of angular momentumTransport of angular momentum
within starswithin stars
Patrick Eggenberger
Département d’Astronomie de l’Université de Genève
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PLATO Mission Conference 2017 2
• Helioseismic measurements
— Problem with shellular rotation Pinsonneault et al. 1989; Chaboyer et al. 1995; Talon et al. 1997; Eggenberger et al. 2005; Turck-Chièze et al. 2010
Garcia et al. 2007
The solar rotation profileThe solar rotation profile
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PLATO Mission Conference 2017 3
Eggenberger et al. 2005
The solar rotation profileThe solar rotation profile
• Effects of magnetic fields
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PLATO Mission Conference 2017 4Charbonnel & Talon 2005
The solar rotation profileThe solar rotation profile
• Effects of internal gravity waves
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PLATO Mission Conference 2017 5
• Impact of MS angular momentum transport on exoplanets
Asteroseismology of MS starsAsteroseismology of MS stars
Eggenberger et al. 2010
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PLATO Mission Conference 2017 6
• Solar-like oscillations in MS stars
mean internal rotation from rotational splittings +
independent measurements of surface rotation rates
Asteroseismology of MS starsAsteroseismology of MS stars
Benomar et al. 2015 Nielsen et al. 2015
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PLATO Mission Conference 2017 7
• More massive MS stars
- Slowly rotating δ Scuti/γ Dor and SPB stars : ~ SB rotation (Kurtz et al. 2014;
Saio et al. 2015; Schmid et al. 2015; Murphy et al. 2016; Triana et al. 2015; Kallinger et al. 2017)
- SB rotation also for faster rotating MS stars? (Van Reeth et al. 2016; Ouazzani et al. 2017)
- β Ceph stars : non-rigid rotation with Ωcore ~ 3 Ωenv (Aerts et al. 2003; Dupret et al. 2004;
Ausseloos et al. 2004; Pamyatnykh et al. 2004) or compatible with SB rotation (Briquet et al. 2007)
Asteroseismology of MS starsAsteroseismology of MS stars
M = 1.2 M
M = 1.5 M
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PLATO Mission Conference 2017 8
Impact of post-MS angular momentum transport
on planet engulfment
AM exchange with the planet
+ internal transport of AM
Asteroseismology of red giantsAsteroseismology of red giants
Privitera et al. 2016
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PLATO Mission Conference 2017 9
Impact of post-MS angular momentum transport
on planet engulfment
High surface magnetic fields + impact of magnetic braking
Asteroseismology of red giantsAsteroseismology of red giants
Privitera et al. 2016
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PLATO Mission Conference 2017 10
Rotational splittings for solar-like oscillations in red giants
- Mixed modes in KIC 8366239 (Beck et al. 2012): 1.5 M with Z
Beck et al. 2012
Asteroseismology of red giantsAsteroseismology of red giants
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PLATO Mission Conference 2017 11
Mixed modes in the red giant KIC 8366239
- Additional mechanism for the transport of angular momentum:
δνrotwings/δνrot
centre = 1.5
⇒ νadd = 3⋅104 cm2 s-1
see study by Goupil et al. (2013)
Eggenberger, Montalban & Miglio 2012
Asteroseismology of red giantsAsteroseismology of red giants
Eggenberger et al. 2012
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PLATO Mission Conference 2017 12
KIC 7341231: a low-mass red giant
- Internal rotation (Deheuvels et al. 2012)
Ωc = 710 ± 51 nHz
Ωs < 150 ± 19 nHz
- Negligible impact of the
rotational history on νadd
(AM transport and
surface braking by
magnetized winds
during MS and PMS):
νadd=1⋅103-1.3⋅104 cm2 s-1
Asteroseismology of red giantsAsteroseismology of red giants
Eggenberger et al. 2017
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PLATO Mission Conference 2017 13
Kepler-56
- Precise estimates of
both core and surface
rotation rates (Huber et al. 2013)
νadd= 1.4 ± 0.1 ⋅ 104 cm2 s-1
νadd when M
Asteroseismology of red giantsAsteroseismology of red giants
rot only: Vi=20 km/s
rot only: Vi=1 km/s νadd=1·104 cm2/s νadd=3·104 cm2/s
Vi=20 km/sVi=25 km/s
Vi=30 km/sVi=40 km/s
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PLATO Mission Conference 2017 14
Rotational splittings for 6 Kepler subgiants and young RGs
- Core and surface rotation rates precisely determined
- Increase of differential rotation when evolution proceeds?
Deheuvels et al. 2014
Asteroseismology of red giantsAsteroseismology of red giants
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PLATO Mission Conference 2017 15
Location of the angular velocity gradient
- KIC 4448777 (Di Mauro et al. 2016) + 2 subgiants (Deheuvels et al. 2014)
- δν/δνmax : differential rotation in the radiative zone (Klion & Quataert 2017)
Asteroseismology of red giantsAsteroseismology of red giants
Di Mauro et al. 2016
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PLATO Mission Conference 2017 16
Core rotation rates for a large number of evolved stars
- Sample of Mosser et al. (2012) + Deheuvels et al. (2014)
Asteroseismology of red giantsAsteroseismology of red giants
Deheuvels et al. 2014
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PLATO Mission Conference 2017 17
Core rotation rates for a large number of evolved stars
- Evolution of core rotation rates: red giants
Asteroseismology of red giantsAsteroseismology of red giants
Spada et al. 2016
!
D = D0
"rad
"env
#
$ %
&
' (
)
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PLATO Mission Conference 2017 18
Core rotation rates for a large number of evolved stars
- Red giants burning helium in non-degenerate conditions
Asteroseismology of red giantsAsteroseismology of red giants
Tayar & Pinsonneault 2013
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PLATO Mission Conference 2017 19
Physical nature of the missing transport mechanism
- Modelling of turbulence (Marques et al. 2013)
Asteroseismology of red giantsAsteroseismology of red giants
Increase Increase of of DDhh and and DDshearshear
Standard modelStandard model
Marques et al. 2013
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PLATO Mission Conference 2017 20
Physical nature of the missing transport mechanism
- Tayler-Spruit dynamo:
predicted transport not
efficient enough (Cantiello et al. 2014)
- IGW generated by turbulent pressure: not efficient (Fuller et al. 2014)
- IGW generated by penetrative convection: not efficient for red
giants but efficient for subgiants (Pinçon et al. 2017)
Asteroseismology of red giantsAsteroseismology of red giants
Cantiello et al. 2014
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PLATO Mission Conference 2017 21
Physical nature of the missing transport mechanism
- Transport of angular momentum by mixed modes
Asteroseismology of red giantsAsteroseismology of red giants
Belkacem et al. 2015
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PLATO Mission Conference 2017 22
Additional mechanism for the transport of angular momentum
− Needed for the Sun and slowly rotating low-mass MS stars.
Also needed for more massive/faster rotating MS stars?
− Needed for subgiants and red giants
Efficiency and physical nature of the additional mechanism
− For subgiants and red giants: νadd can be precisely determined
− Red giants: νadd with mass and evolutionary state
− Magnetic fields: fossil fields? MHD instabilities: νadd ok with AMRI
− IGW: not for red giants. subgiants: penetrative convection
− Mixed modes: efficient for evolved red giants
SummarySummary