اخترلرزهشناسی (به انگلیسی: Asteroseismology) یا (به انگلیسی: stellar seismology) شاخهای از ستارهشناسی و یکی از روشهای بررسی در اخترفیزیک است که به کمک روشهای دانش لرزهشناسی به بررسی لرزههای نور ستارگان؛ (به غیر از خورشید که در آن صورت لرزهشناسی خورشیدی (به انگلیسی: Helioseismology) نامیده میشود)، از راه اندازهگیری دقیق نوسان نور آنها میپردازد.
در زمین و در دیگر اجسام جامد فضایی قابل دسترس- زلزله شناسان برای بررسی ساختار درونی این اجسام از اندازهگیری نوسانهای زلزله؛ که گاهی خود آن لرزهها را ایجاد میکنند، بهره میگیرند. این روش در مورد ستارگان نمیتواند بکار گرفته شود.
نوسانهای مختلف٫ ژرفای نفوذی مختلفی دارند. با بهرهگیری از این واقعیت میتوان با گزینش درست نوسان٫ در عمق دلخواه ستاره نفوذ کرد یا برعکس به چبود منشأ نوسانهای پدید آمده پی برد. با بهرهوری از این پی آمد است که این ابزار میتواند دستیابی به این دانستههای دور از دسترس را برای ما فراهم کند.
با کمک این شاخه از اخترشناسی میتوان در نهایت به چگونگی ساختار درونی ستارگان با بررسی لرزشهای تپش گونه ئی که دارند پی برد. بازخوانی طیف فرکانسی این لرزهها٫ ساختارهای درونی ستاره را آشکار میسازد. علاوه بر این؛ نیاز اخترلرزهشناسی به دقت و تفکیکپذیری بسیار بالای دادهها در همه روند کار، ویژگیهای دانسته پیشین دربارهٔ ستارگان را بسیار دقیق تر و کامل تر کردهاست.
Asteroseismology or astroseismology is the study of oscillations in stars. Because a star's different oscillation modes are sensitive to different parts of the star, they inform astronomers about the internal structure of the star, which is otherwise not directly possible from overall properties like brightness and surface temperature. Asteroseismology is closely related to helioseismology, the study of stellar oscillations specifically in the Sun. Though both are based on the same underlying physics, more and qualitatively different information is available for the Sun because its surface can be resolved.
By linearly perturbing the equations defining the mechanical equilibrium of a star (i.e. mass conservation and hydrostatic equilibrium) and assuming that the perturbations are adiabatic, one can derive a system of four differential equations whose solutions give the frequency and structure of a star's modes of oscillation. The stellar structure is usually assumed to be spherically symmetric, so the horizontal (i.e. non-radial) component of the oscillations is described by spherical harmonics, indexed by an angular degree and azimuthal order . In non-rotating stars, modes with the same angular degree must all have the same frequency because there is no preferred axis. The angular degree indicates the number of nodal lines on the stellar surface, so for large values of , the opposing sectors roughly cancel out, making it difficult to detect light variations. As a consequence, modes can only be detected up to an angular degree of about 3 in intensity and about 4 if observed in radial velocity.
By additionally assuming that the perturbation to the gravitational potential is negligible (the Cowling approximation) and that the star's structure varies more slowly with radius than the oscillation mode, the equations can be reduced approximately to one second-order equation for the radial component of the displacement eigenfunction ,
where is the radial co-ordinate in the star, is the angular frequency of the oscillation mode, is the sound speed inside the star, is the Brunt-Vaisala or buoyancy frequency and is the Lamb frequency. The last two are defined by
respectively. By analogy with the behaviour of simple harmonic oscillators, this implies that oscillating solutions exist when the frequency is either greater or less than both and . We identify the former case as high-frequency pressure modes (p-modes) and the latter as low-frequency gravity modes (g-modes).
This basic separation allows us to determine (to reasonable accuracy) where we expect what kind of mode to resonate in a star. By plotting the curves and (for given ), we expect p-modes to resonate at frequencies below both curves or frequencies above both curves.
Under fairly specific conditions, some stars have regions where heat is transported by radiation and the opacity is a sharply decreasing function of temperature. This opacity bump can drive oscillations through the -mechanism (or Eddington valve). Suppose that, at the beginning of an oscillation cycle, the stellar envelope has contracted. By expanding and cooling slightly, the layer in the opacity bump becomes more opaque, absorbs more radiation, and heats up. This heating causes expansion, further cooling and the layer becomes even more opaque. This continues until the material opacity stops increasing so rapidly, at which point the radiation trapped in the layer can escape. The star contracts and the cycle prepares to commence again. In this sense, the opacity acts like a valve that traps heat in the star's envelope.
Pulsations driven by the -mechanism are coherent and have relatively large amplitudes. It drives the pulsations in many of the longest-known variable stars, including the Cepheid and RR Lyrae variables.
In stars with surface convection zones, turbulent fluids motions near the surface simultaneously excite and damp oscillations across a broad range of frequency. Because the modes are intrinsically stable, they have low amplitudes and are relatively short-lived. This is the driving mechanism in all solar-like oscillators.
If the base of a surface convection zone is sharp and the convective timescales slower than the pulsation timescales, the convective flows react too slowly perturbations[clarification needed] that can build up into large, coherent pulsations. This mechanism is known as convective blocking and is believed to drive pulsations in the Doradus variables.
Observations from the Kepler satellite revealed eccentric binary systems in which oscillations are excited during the closest approach. These systems are known as heartbeat stars because of the characteristic shape of the lightcurves.
Types of oscillators
Because solar oscillations are driven by near-surface convection, any stellar oscillations caused similarly are known as solar-like oscillations and the stars themselves as solar-like oscillators. However, solar-like oscillations also occur in evolved stars (subgiants and red giants), which have convective envelopes, even though the stars are not Sun-like.
Cepheid variables are one of the most important classes of pulsating star. They are core-helium burning stars with masses above about 5 solar masses. They principally oscillate at their fundamental modes, with typical periods ranging from days to months. Their pulsation periods are closely related to their luminosities, so it is possible to determine the distance to a Cepheid by measuring its oscillation period, computing its luminosity, and comparing this to its observed brightness.
Cepheid pulsations are excited by the kappa mechanism acting on the second ionization zone of helium.
RR Lyrae variables
RR Lyraes are similar to Cepheid variables but of lower metallicity (i.e. Population II) and much lower masses (about 0.6 to 0.8 time solar). They are core helium-burning giants that oscillate in one or both of their fundamental mode or first overtone. The oscillation are also driven by the kappa mechanism acting through the second ionization of helium. Many RR Lyraes, including RR Lyrae itself, show long period amplitude modulations, known as the Blazhko effect.
Delta Scuti and Gamma Doradus stars
Delta Scuti variables are found roughly where the classical instability strip intersects the main sequence. They are typically A- to early F-type dwarfs and subgiants and the oscillation modes are low-order radial and non-radial pressure modes, with periods ranging from 0.25 to 8 hours and magnitude variations anywhere between. Like Cepheid variables, the oscillations are driven by the kappa mechanism acting on the second ionization of helium.
SX Phoenicis variables are regarded as metal-poor relatives of Delta Scuti variables.
Gamma Doradus variables occur in similar stars to the red end of the Delta Scuti variables, usually of early F-type. The stars show multiple oscillation frequencies between about 0.5 and 3 days, which is much slower than the low-order pressure modes. Gamma Doradus oscillations are generally thought to be high-order gravity modes, excited by convective blocking.
Rapidly oscillating Ap (roAp) stars
Rapidly oscillating Ap stars have similar parameters to Delta Scuti variables, mostly being A- and F-type, but they are also strongly magnetic and chemically peculiar (hence the p spectral subtype). Their dense mode spectra are understood in terms of the oblique pulsator model: the modes frequencies are modulated by the magnetic field, which is not necessarily aligned with the star's rotation (as is the case in the Earth). The oscillation modes have frequencies around 1500 μHz and amplitudes of a few mmag.
Slowly-pulsating B stars and Beta Cephei variables
Slowly-pulsating B (SPB) stars are B-type stars with oscillation periods of a few days, understood to be high-order gravity modes excited by the kappa mechanism. Beta Cephei variables are slightly hotter (and thus more massive), also have modes excited by the kappa mechanism and additionally oscillate in low-order gravity modes with periods of several hours. Both classes of oscillators contain only slowly-rotating stars.
Variable subdwarf B stars
Subdwarf B (sdB) stars are in essence the cores of core-helium burning giants who have somehow lost most of their hydrogen envelopes, to the extent that there is no hydrogen burning shell. They have multiple oscillation periods that range between about 1 and 10 minutes and amplitudes anywhere between 0.001 and 0.3 mag in visible light. The oscillations are low-order pressure modes, excited by the kappa mechanism acting on the iron opacity bump.
White dwarfs are characterized by spectral type, much like ordinary stars, except that the relationship between spectral type and effective temperature does not correspond in the same way. Thus, white dwarfs are known by types DO, DA and DB. Cooler types are physically possible but the Universe is too young for them to have cooled enough. White dwarfs of all three types are found to pulsate. The pulsators are known as GW Virginis stars (DO variables, sometimes also known as PG 1159 stars), V777 Herculis stars (DB variables) and ZZ Ceti stars (DA variables). All pulsate in low-degree, high-order g-modes. The oscillation periods broadly decrease with effective temperature, ranging from about 30 min down to about 1 minute. GW Virginis and ZZ Ceti stars are thought to be excited by the kappa mechanism; V777 Herculis stars by convective blocking.
A number of past, present and future spacecraft have asteroseismology studies as a significant part of their missions (order chronological).