Core-Envelope Rotational Misalignment in Kepler-56

NHFP Symposium | Slides at hyad.es/talks

Joel Ong
Hubble Fellow, Univ. of Hawaiʻi at Mānoa

September 19, 2024

Seismology and Rotation

(sun-like star)

Photometric \(P_\text{rot}\):
\(\ll 1\ \mu\text{Hz}\)
\(\downarrow\)

Spectroscopic \(V \sin i\):
\(\sim \text{PHz}\) regime \(\to\)

Power spectra of MDI dopplergrams

Cool main-sequence stars exhibit p-modes:
pure pressure waves.

Mode frequency measurements constrain
internal structure and rotation.

Two rotational axes?

Why???

  • Stars tend to have (and interact with) companions: binaries, planetary systems, engulfments…
  • Seismic rotational measurements indicate anomalies?

How???

Pressure waves (p-modes)
propagate isotropically.

Buoyancy waves (g-modes)
propagate anisotropically.

\[b_i(r) = b_i \int_0^r K_i(r') \mathrm d r'\]

Gravitoacoustic “mixed” modes probe radial differential rotation
in two zones (core vs. envelope).

Cumulative sensitivity \(b(r)\)

pure g-mode pure p-mode

Kepler-56

\[b_i(r) = b_i \int_0^r K_i(r') \mathrm d r'\]

Mixed modes probe radial differential rotation
in two zones (core vs. envelope).

Cumulative sensitivity \(b(r)\)

\[b_i(r) = b_i \int_0^r K_i(r') \mathrm d r'\]

Even the most p-dominated mixed modes
are sensitive to core rotation!

Cumulative sensitivity \(b(r)\)

What does this mean???

  • One less known misaligned multiplanet system
    • Implications for orbital architectures?
  • What about other notionally envelope-counterrotating stars?
  • Constraints on realignment \(\mathcal{Q}\) and/or torque mechanisms?

Asteroseismic Diagnostics of
Core-Envelope Misalignment

Key prediction: apparent inclination angle
should vary from multiplet to multiplet.

Application to Kepler-56 suggests internal misalignment.
Follow-up Rossiter-McLaughlin RV measurements
may further constrain geometry.

\[\mathrm{j}\mathrm{o}\mathrm{e}\mathrm{l}\mathrm{o}\mathrm{n}\mathrm{g}\ \text{@}\ \text{hawaii}.\text{edu}\]

Backup Slides

Parameterising Misalignment

Euler Angles

Matrix Construction

Angular Momentum Matrices

\(\forall \ell, \exists (2\ell + 1) \times (2\ell + 1)\) matrices
\(\mathbf{J}_x^\ell\), \(\mathbf{J}_y^\ell\), \(\mathbf{J}_z^\ell\) satisfying commutation relations
\(\left[\mathbf{J}_i, \mathbf{J}_j\right] = -i\epsilon_{ijk}\mathbf{J}_k\), with
\(\mathbf{J}_z \hat{=} \mathrm{diag}(-\ell, -\ell + 1 \ldots \ell - 1, \ell).\)

Example: \(\ell = 1\)

\[\small\mathbf{J}_x \hat{=} {1 \over \sqrt{2}}\begin{bmatrix}0 & 1 & 0 \\ 1 & 0 & 1 \\ 0 & 1 & 0\end{bmatrix}; \mathbf{J}_y \hat{=} {1 \over \sqrt{2}}\begin{bmatrix}0 & i & 0 \\ -i & 0 & i \\ 0 & -i & 0\end{bmatrix}; \mathbf{J}_z \hat{=} \begin{bmatrix}-1 & 0 & 0 \\ 0 &0 &0 \\ 0& 0 &1\end{bmatrix}.\]

Rotation as an Eigenvalue Problem

For fixed \(m\) (to leading order):

\[\left(-\mathbf{\Omega}_0^2 + 2 \omega m \mathbf{R} + \omega^2 \mathbf{\Delta}\right)\mathbf{c} = 0\]

For fixed \(n\) (to leading order):

\[(-\omega_0^2 \mathbb{1}_{2\ell+1} + 2 \omega \mathbf{J}_z R_{n,n} + \omega^2 \mathbb{1}_{2\ell+1})\mathbf{y} = 0\]

Combined Angular Momentum Operator
(Aligned Case)

\[\vec{\xi}_{n\ell m}(r, \theta, \varphi) = \vec{\xi}_{n\ell}(r) Y_\ell^m(\theta, \phi) \iff \underbrace{\tilde{R}_{n, n', m, m'} = R_{n,n'} J_{m,m'}}_{\text{this is a }\textbf{tensor product}!}\]

\[\implies \left(-\mathbf{\Omega_0}^2 \otimes \mathbb{1}_{2\ell+1} + 2 \omega \underbrace{\mathbf{R} \otimes \mathbf{J}_z}_{\tilde{\mathbf{R}}} + \omega^2 \mathbf{\Delta} \otimes \mathbb{1}_{2\ell+1}\right)\mathbf{x} = 0\]

The Misaligned Angular Momentum Operator

Let’s associate with each mass shell at \(r\) both \(\Omega(r)\)
(as is customary), and also an axis \(\hat{\mathbf{n}}(r) =\sum_i n_i \mathbf{e}_i\).

\[\small \begin{aligned} \mathbf{R}_{n\ell, n\ell} &= b_{n\ell}\int {\mathbf{d}^\ell}^\dagger(\beta(r)) \Omega(r) \mathbf{J}_z {\mathbf{d}^\ell}(\beta(r))\ K(r)\ \mathrm{d} r\\ &= b_{n\ell}\int \Omega(r) (\hat{\mathbf{n}} \cdot \vec{\mathbf{J}})\ K(r)\ \mathrm{d} r\\ &= \boxed{b_{n\ell}\left(\int \vec{\mathbf{\Omega}}(r) K(r)\ \mathrm{d} r\right) \cdot \vec{\mathbf{J}}}. \end{aligned} \]

\[ \boxed{\tilde{\mathbf{R}} = \int \mathbf{K}\otimes\left(\Omega_\text{rot}(r)\ \hat{\mathbf{n}}\cdot \vec{\mathbf{J}}\right)\ \mathrm{d}r} \]

\(\implies\) For each mode, AM matrix is
specified by usual vector addition.

Mixed Modes

We only assume that the pure p- and g-mode solutions
are separately amenable to separation of variables;
the mixed-mode eigenfunctions need not be.

\[ \small \left(\begin{bmatrix} {\color{grey}\mathbf{L}_{\pi\pi}} & \mathbf{L}_{\pi\gamma} \\ \mathbf{L}_{\pi\gamma}^T & {\color{red}\mathbf{L}_{\gamma\gamma}} \end{bmatrix} \otimes \mathbb{1}_{2\ell+1} + 2 \omega \begin{bmatrix} {\color{forestgreen}\tilde{\mathbf{R}}_\pi} & 0 \\ 0 & {\color{forestgreen}\tilde{\mathbf{R}}_\gamma}\end{bmatrix} + \omega^2 \begin{bmatrix} \mathbb{1} & \mathbf{D} \\ \mathbf{D}^T & \mathbb{1} \end{bmatrix} \otimes \mathbb{1}_{2\ell+1} \right)\mathbf{x} = 0. \]

Mode mixing yields avoided crossings
between multiplet components of identical \(m\)

(cf. Mosser+ 2012, Ouazzani+ 2013, Deheuvels+ 2017)

\(\beta = 0\)

\(\beta = {\pi\over10}\)

\(\beta = {\pi\over2}\)

\(\beta = \pi\)

More Kepler-56

R-M Misalignment

Hjorth et al. 2021: Extreme misalignment angles are possible even in a coplanar configuration