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Recent asteroseismic observations by the Kepler space mission have revealed the dip fine structure in the period-spacing versus period diagram of rapidly rotating γ Doradus stars. Following the successful reproduction of the dip structure by numerical calculations in previous studies, we present in this paper the physical mechanism of how the dip is formed as a result of the interaction between the gravito-inertial waves in the radiative envelope and the pure inertial waves in the convective core. We analytically describe the wave solutions in both of the radiative envelope and the convective core, and match them at the interface to construct an eigenmode. We have found from the analysis the following points: the dip structure is mainly controlled by a parameter that has an inverse correlation with Brunt–Väisälä frequency at the interface; the depth and the width of the dip is shallower and larger, respectively, as the parameter gets large; the shape of the dip can be approximated by the Lorentzian function; the period at the central position of the dip is equal to or slightly smaller than that of the involved pure inertial mode in the convective core. We have also understood based on the evolutionary models of main-sequence stars that the parameter is inversely correlated with the chemical composition gradient at the convective-core boundary. The dip structure thus would provide information about the poorly-understood physical processes, such as diffusion, convective overshooting and rotational mixing, around the boundary between the convective core and the radiative envelope. [ABSTRACT FROM AUTHOR]

The relation of period spacing (Δ P) versus period (P) of dipole prograde g modes is known to be useful to measure rotation rates in the g-mode cavity of rapidly rotating γ Dor and slowly pulsating B (SPB) stars. In a rapidly rotating star, an inertial mode in the convective core can resonantly couple with g-mode propagative in the surrounding radiative region. The resonant coupling causes a dip in the P  – Δ P relation, distinct from the modulations due to the chemical composition gradient. Such a resonance dip in Δ P of prograde dipole g modes appears around a frequency corresponding to a spin parameter 2 f rot(cc)/ ν co-rot ∼8–11 with f rot(cc) being the rotation frequency of the convective core and ν co-rot the pulsation frequency in the co-rotating frame. The spin parameter at the resonance depends somewhat on the extent of core overshooting, central hydrogen abundance, and other stellar parameters. We can fit the period at the observed dip with the prediction from prograde dipole g modes of a main-sequence model, allowing the convective core to rotate differentially from the surrounding g-mode cavity. We have performed such fittings for 16 selected γ Dor stars having well-defined dips, and found that the majority of γ Dor stars we studied rotate nearly uniformly, while convective cores tend to rotate slightly faster than the g-mode cavity in less evolved stars. [ABSTRACT FROM AUTHOR]

Strong magnetic fields in chemically peculiar A-type (Ap) stars typically suppress low-overtone pressure modes (p modes) but allow high-overtone p modes to be driven. KIC 11296437 is the first star to show both. We obtained and analysed a Subaru spectrum, from which we show that KIC 11296437 has abundances similar to other magnetic Ap stars, and we estimate a mean magnetic field modulus of 2.8 ± 0.5 kG. The same spectrum rules out a double-lined spectroscopic binary, and we use other techniques to rule out binarity over a wide parameter space, so the two pulsation types originate in one δ Sct–roAp hybrid pulsator. We construct stellar models depleted in helium and demonstrate that helium settling is second to magnetic damping in suppressing low-overtone p modes in Ap stars. We compute the magnetic damping effect for selected p and g modes, and find that modes with frequencies similar to the fundamental mode are driven for polar field strengths ≲4 kG, while other low-overtone p modes are driven for polar field strengths up to ∼1.5 kG. We find that the high-order g modes commonly observed in γ Dor stars are heavily damped by polar fields stronger than 1–4 kG, with the damping being stronger for higher radial orders. We therefore explain the observation that no magnetic Ap stars have been observed as γ Dor stars. We use our helium-depleted models to calculate the δ Sct instability strip for metallic-lined A (Am) stars, and find that driving from a Rosseland mean opacity bump at ∼5 × 104 K caused by the discontinuous H-ionization edge in bound-free opacity explains the observation of δ Sct pulsations in Am stars. [ABSTRACT FROM AUTHOR]

The rotation rates in the interior and at the surface is determined for the 22 main-sequence stars with masses between 1.0 and 1.6 M⊙. The average interior rotation is measured using asteroseismology, while the surface rotation is measured by the spectroscopic v sin i or the periodic light variation due to surface structures, such as spots. It is found that the difference between the surface rotation rate determined by spectroscopy and the average rotation rate for most of stars is small enough to suggest that an efficient process of angular momentum transport operates during and/or before the main-sequence stage of stars. By comparing the surface rotation rate measured from the light variation with those measured by spectroscopy, we found hints of latitudinal differential rotation. However, this must be confirmed by a further study because our result is sensitive to a few data points. [ABSTRACT FROM PUBLISHER]

We have found a rotationally split series of core g-mode triplets and surface p-mode multiplets in a main-sequence F star, KIC 9244992. Comparison with models shows that the star has a mass of about 1.45 M⊙, and is at an advanced stage of main-sequence evolution in which the central hydrogen abundance mass fraction is reduced to about 0.1. This is the second case, following KIC 11145123, of an asteroseismic determination of the rotation of the deep core and surface of an A-F main-sequence star. We have found, essentially model independently, that the rotation near the surface, obtained from p-mode splittings, is 66 d, slightly slower than the rotation of 64 d in the core, measured by g-mode splittings. KIC 9244992 is similar to KIC 11145123 in that both are near the end of main-sequence stage with very slow and nearly uniform rotation. This indicates the angular momentum transport in the interior of an A-F star during the main-sequence stage is much stronger than that expected from standard theoretical formulations. [ABSTRACT FROM AUTHOR]

We have discovered rotationally split core g-mode triplets and surface p-mode triplets and quintuplets in a terminal age main-sequence A star, KIC 11145123, that shows both δ Sct p-mode pulsations and γ Dor g-mode pulsations. This gives the first robust determination of the rotation of the deep core and surface of a main-sequence star, essentially model independently. We find its rotation to be nearly uniform with a period near 100 d, but we show with high confidence that the surface rotates slightly faster than the core. A strong angular momentum transfer mechanism must be operating to produce the nearly rigid rotation, and a mechanism other than viscosity must be operating to produce a more rapidly rotating surface than core. Our asteroseismic result, along with previous asteroseismic constraints on internal rotation in some B stars, and measurements of internal rotation in some subgiant, giant and white dwarf stars, has made angular momentum transport in stars throughout their lifetimes an observational science. [ABSTRACT FROM PUBLISHER]

We analyse the rosette modes of oscillations in rotating stars, which are characterised by rosette patterns of the kinetic-energy distribution on the meridional plane. Following our previous argument that these modes are generated by the rotation-induced interaction among eigenmodes with almost the same frequency, we discuss the structure of the rosette patterns base on the JWKB analysis. We also demonstrate that there exist nonaxisymmetric rosette modes. [ABSTRACT FROM PUBLISHER]

An asymptotic analysis is developed to describe rosette modes of oscillations in rotating stars, which have been recently discovered in numerical computations. The name of the modes comes from characteristic rosette patterns of the distributions of the kinetic-energy density on the meridional plane. As have been shown in the previous papers in this series, the physical reason for the formation of these modes is the rotation-induced interaction among several gravity modes with almost the same frequencies and successive spherical degrees of the same parity. This formation process is described in the framework of the quasi-degenerate perturbation theory. In this paper, the matrix eigenvalue problem, which appears in the perturbation analysis, is solved analytically, using asymptotic expressions of eigenfunctions, which are obtained by assuming that the wavelength of oscillations in the horizontal direction is sufficiently small. By further assuming that the number of interacting modes is large, simple expressions of the eigenfunctions and eigenfrequencies of rosette modes are obtained. Because these expressions can describe the essential part of characteristics of rosette modes, they are useful in understanding general properties of rosette modes that are common to any equilibrium structure. [ABSTRACT FROM PUBLISHER]

Our previous analysis of axisymmetric rosette modes of oscillations in rigidly rotating stars is extended to nonaxisymmetric modes. The rosette modes, which have peculiar eigenfunctions, are formed by interaction among g modes having close frequencies with the particular rules regarding radial orders and spherical degrees. Such interaction is caused by the second-order effect of the Coriolis force. For nonaxisymmetric cases, the first-order rotation effect, which is proportional to the azimuthal order and the rotation frequency, tends to work against the formation of rosette modes. It is, however, found that the poisoning effect is not so serious in many cases that nonaxisymmetric rosette modes are present. The difference between prograde and retrograde modes is discussed. [ABSTRACT FROM AUTHOR]