magnetohydrodynamic simulations of stellar differential rotation and meridional circulation
DESCRIPTION
Magnetohydrodynamic simulations of stellar differential rotation and meridional circulation (submitted to A&A, arXiv:1407.0984). Bidya Binay Karak (Nordita fellow) In collaboration with Petri J. Kapyla, Maarit J. Kapyla, and Axel Brandenburg. Internal solar rotation from helioseismology. - PowerPoint PPT PresentationTRANSCRIPT
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Magnetohydrodynamic simulations of stellar differential
rotation and meridional circulation
(submitted to A&A, arXiv:1407.0984)
Bidya Binay Karak
(Nordita fellow)
In collaboration with Petri J. Kapyla, Maarit J. Kapyla, and Axel Brandenburg
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Internal solar rotation from helioseismology
Gilman & Howe (2003)
=>Solar-like differential rotationobserved in rapidly rotating dwarfs (e.g. Collier Cameron 2002)
When polar regions rotate faster than equator regions is called anti-solar differential rotation.
-observed in slowly rotating stars (e.g., K giant star HD 31993; Strassmeier et al. 2003; Weber et al. 2005).
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Transition from solar-like to anti-solar differential rotation in simulations (Gilman 1978; Brun & Palacios 2009; Chan 2010;Kapyla et al. 2011; Guerrero et al. 2013; Gastine et al. 2014)
Independent of model setup.
Gastine et al. (2014)
Solar-like
Anti-solar
Solar-like
Anti-solar
(Gilman 1977)
Guerrero et al. (2013)
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Bistability of differential rotation Observed in many HD simulations
Gastine et al. (2014)from Boussinesq convection.
Kapyla et al. (2014)
in fully compressiblesimulations
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We carry out a set of full MHD simulationsModel equations
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Computations are performed in spherical wedge geometry:
0 00.72 0.97 ,15 165 ,02
R r R
We performed several simulations by varying the rotational influence on the convection.
We regulate the convective velocities by varying the amount of heat transported by thermal conduction, turbulent diffusion, and resolved convection
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MHD
Co = 1.34, 1.35, 1.44, 1.67, 1.75
Rotational effect on the convection is increased
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MHD
Co = 1.34, 1.35, 1.44, 1.67, 1.75
Rotational effect on the convection is increased
HD
443430
325
503
430
315
918
430
261
939
430
263
980
430
265
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Identifying the transition of differential rotation
No evidence of bistability!Gastine et al. (2014)Kapyla et al. (2014)
Magnetic field helps to produce more solar-like differential rotation
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A-S diff. rot. S-L diff. rot.
Meridional circulation
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Azimuthally averaged toroidal field near the bottom of SCZ
Runs produce anti-solardifferential rotation
Runs produce solar-like differential rotation
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Temporal variations from Run AFromRun A(ASDiff.Rot)
Variation:~ 50%
~ 6%
~ 75%
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How the variation in large-scale flow comes?
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Variation of Lorentz forces over magnetic cycle Maximum Minimum
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Angular momentum fluxes (e.g., Brun et al. 2004; Beaudoin et al. 2013)
(Rudiger 980, 1989)
Reynolds stress
Maxwell stress
Coriolis force
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Run A (produces anti-solar differential rotation)
Run E (produces solar-like differential rotation)Reynolds Viscosity Lambda effect
cm2/s
cm2/s
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Run E (produces solar-like differential rotation)
Run A (produces anti-solar differential rotation)
Meridonal circulation Maxwell stress Mean-magnetic part
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Temporal variation: From Run A (solar-like diff. rot.)
Reynolds stress Meridional Maxwell stress Mean-magnetic circulation part
Max
Min
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Thanks for your attention!
BTW, my NORDITA fellowship will end next year mid, so looking for next post doc position.
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Drivers of the meridional circulation(Ruediger 1989; Kitchatinov & Ruediger 1995; Miesch & Hindman 2011)
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Identifying the transition of differential rotation
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Boundary conditions
For magnetic field: Perfect conductor at latitudinal boundaries and lower radial boundary. Radial field condition at the outer boundary
On the latitudinal boundaries we assume that the density and entropy have vanishing first derivatives.
On the upper radial boundary we apply a black body condition:
We add a small-scale low amplitude Gaussian noise as initial conditionfor velocity and magnetic field
For velocity field: Radial and latitudinal boundaries are impenetrable and stress-free
Initial stateisoentropic
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Boundary conditions
For magnetic field: Perfect conductor at latitudinal boundaries and lower radial boundary. Radial field condition at the outer boundary
On the latitudinal boundaries we assume that the density and entropy have vanishing first derivatives.
On the upper radial boundary we apply a black body condition:
For velocity field: Radial and latitudinal boundaries are impenetrable and stress-free
Computations are performed in spherical wedge geometry:
We use pencil-code.
0 00.72 0.97 ,15 165 ,02
R r R
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FromRun E(SLDiff Rot)
Variation:~ 40%
~ 4%
~ 50%
~ 60%