Identification of Inertial Modes in the Solar Convection Zone

Triana, S. A.; Gómez, Gutiérrez; Barik, Ankit; Rekier, J.

doi:10.3847/2041-8213/ac7dac

Cited by 18 publications

(24 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In discretizing the operators, we follow Triana et al (2022) and split our analysis into two sets of modes: one for which the toroidal stream function V is symmetric about the equator, and another for which it is antisymmetric. In the symmetric case, only the spherical harmonic degrees ℓ = m, m + 2, m + 4 L contribute to V; whereas in the antisymmetric case, the contribution comes from ℓ = m + 1, m + 3, m + 5 L .…”

Section: Numerical Implementationmentioning

confidence: 99%

“…that features in the definition of the inner product with respect to which the polynomials are orthogonal, and this differs from the degree q of the polynomial. This approach is similar to that used by Triana et al (2022). Such a sparse representation makes the evaluation of the operator matrices computationally inexpensive, and permits a purely spectral approach, as opposed to a pseudospectral one.…”

Section: Numerical Implementationmentioning

confidence: 99%

“…A few comments are in order to explain how our method is similar to and distinct from the existing approaches. Several numerical investigations into the spectrum of Rossby waves have recently been carried out, notably those by Bekki et al (2022) and Triana et al (2022). The former set of authors use a finite-difference approach, whereas the latter use a spectral approach.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Spectral Solver for Solar Inertial Waves

Bhattacharya¹,

Hanasoge

2023

ApJS

View full text Add to dashboard Cite

Inertial waves, which are predominantly driven by the Coriolis force, likely play an important role in solar dynamics, and, additionally, they provide a window into the solar subsurface. The latter allows us to infer properties that are inaccessible to the traditional technique of acoustic wave helioseismology. Thus, a full characterization of these normal modes holds the promise of enabling investigations into solar subsurface dynamics. In this work, we develop a spectral eigenvalue solver to model the spectrum of inertial waves in the Sun. We model the solar convection zone as an anelastic medium, and solve for the normal modes of the momentum and energy equations. We demonstrate that the solver can well reproduce the observed mode frequencies and line widths, not only of sectoral Rossby modes, but also of recently observed high-frequency inertial modes. In addition, we believe that the spectral solver is a useful contribution to the numerical methods of modeling inertial modes on the Sun.

show abstract

Section: Numerical Implementationmentioning

confidence: 99%

Section: Numerical Implementationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A Spectral Solver for Solar Inertial Waves

Bhattacharya¹,

Hanasoge

2023

ApJS

View full text Add to dashboard Cite

show abstract

“…Furthermore, Hanson et al (2022) have recently reported additional low-amplitude modes of north-south antisymmetric vorticity near the equator that propagate in a retrograde direction with 8 ≤ m ≤ 14. These modes are also likely inertial modes, according to the simplified linear analysis by Triana et al (2022). Whether these modes are also present in the more realistic solar models has not yet been studied.…”

Section: Other Inertial Modesmentioning

confidence: 99%

Theory of solar oscillations in the inertial frequency range: Amplitudes of equatorial modes from a nonlinear rotating convection simulation

Bekki

Cameron

Gizon

2022

A&A

View full text Add to dashboard Cite

Context. Several types of inertial modes have been detected on the Sun. Properties of these inertial modes have been studied in the linear regime but have not been studied in nonlinear simulations of solar rotating convection. Comparing the nonlinear simulations, the linear theory, and the solar observations is important to better understand the differences between the models and the real Sun. Aims. We wish to detect and characterize the modes present in a nonlinear numerical simulation of solar convection, in particular to understand the amplitudes and lifetimes of the modes. Methods. We developed a code with a Yin-Yang grid to carry out fully-nonlinear numerical simulations of rotating convection in a spherical shell. The stratification is solar-like up to the top of the computational domain at 0.96 R . The simulations cover a duration of about 15 solar years, which is more than the observational length of the Solar Dynamics Observatory (SDO). Various large-scale modes at low frequencies (comparable to the solar rotation frequency) are extracted from the simulation. Their characteristics are compared to those from the linear model and to the observations. Results. Among other modes, both the equatorial Rossby modes and the columnar convective modes are seen in the simulation. The columnar convective modes, with north-south symmetric longitudinal velocity v φ , contain most of the large-scale velocity power outside the tangential cylinder and substantially contribute to the heat and angular momentum transport near the equator. Equatorial Rossby modes with no radial node (n = 0) are also found: They have the same spatial structures as the linear eigenfunctions. They are stochastically excited by convection and have the amplitudes of a few m s −1 and mode linewidths of about 20-30 nHz, which are comparable to those observed on the Sun. We also confirm the existence of the "mixed Rossby modes" between the equatorial Rossby modes with one radial node (n = 1) and the columnar convective modes with north-south antisymmetric v φ in our nonlinear simulation, as predicted by the linear eigenmode analysis. We also see the high-latitude mode with m = 1 in our nonlinear simulation but its amplitude is much weaker than that observed on the Sun.

show abstract

Section: Other Inertial Modesmentioning

confidence: 95%

Theory of solar oscillations in the inertial frequency range

Bekki¹

View full text Add to dashboard Cite

show abstract

Identification of Inertial Modes in the Solar Convection Zone

Cited by 18 publications

References 35 publications

A Spectral Solver for Solar Inertial Waves

A Spectral Solver for Solar Inertial Waves

Theory of solar oscillations in the inertial frequency range: Amplitudes of equatorial modes from a nonlinear rotating convection simulation

Theory of solar oscillations in the inertial frequency range

Contact Info

Product

Resources

About