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1.
I. Yu. Alekseev 《Astrophysics》2005,48(1):20-31
The first results are reported from a search for activity cycles in stars similar to the sun based on modelling their spotting with an algorithm developed at the Crimean Astrophysical Observatory. Of the more than thirty program stars, 10 manifested a cyclical variation in their central latitudes and total starspot area. The observed cycles have durations of 4–15 years, i.e., analogous to the 11 year Schwabe sunspot cycle. Most of the stars have a rough analog of the solar butterfly pattern, with a reduction in the average latitude of the spots as their area increases. A flip-flop effect during the epoch of the maximum average latitude is noted in a number of these objects (e.g., the analog LQ Hya of the young sun or the RS CVn-type variable V711 Tau), as well as a reduction in the photometric rotation period of a star as the spots drift toward the equator, an analog of the differential rotation effect in the sun. Unlike in the sun, the observed spot formation cycles do not correlate uniquely with other indicators of activity— chromospheric emission in the CaII HK lines (Be Cet, EK Dra, Dx Leo), H line emission (LQ Hya, VY Ari, EV Lac), or cyclical flare activity (EV Lac). In V833 Tau, BY Dra, EK Dra, and VY Ari short Schwabe cycles coexist with long cycles that are analogous to the Gleissberg solar cycle, in which the spotted area can approach half the entire area of the star.Translated from Astrofizika, Vol. 48, No. 1, pp. 29–43 (February 2005). 相似文献
2.
J.R. Barnes A. Collier Cameron D.J. James D. Steeghs 《Monthly notices of the Royal Astronomical Society》2001,326(3):1057-1066
We present two images of intermediate and low axial inclination G dwarfs (AP 149 and AP 193) in the young open cluster α Persei, and compare these with previous images of intermediate and high axial inclination objects in this cluster. All stars show starspots at high latitudes, with one star exhibiting a strong polar spot. Although low-latitude features are found on all stars to some degree, the detection of spots on AP 193 is marginal. The apparent difference in starspot morphology from one object to the next is probably the result of a stellar magnetic cycle, although the exact effect on the starspot distribution throughout a cycle is unknown.
Polar spots are found in many Doppler images of rapidly rotating cool stars. In the past, their existence has been called into question, and it has been suggested that they could be the manifestations of NLTE (e.g. chromospheric filling in of line profiles) effects rather than real photospheric features. We assume the polar spots to be real photospheric features, and conclude that the flat-bottomed nature of the profile shape can be attributed to photospheric polar spots. The degree of truncation of the profile depends not only on spot size and strength, but also on the effective foreshortening of the polar region, a function of axial inclination.
H α is in emission on AP 149 which shows a double peak at most phases. The time-series of the profile shows an s-wave pattern as the position of these peaks changes throughout the rotation cycle. We attribute this to coronal clouds located above the stellar surface in synchronous orbit. A maximum-entropy tomogram is derived revealing four distinct emission regions located near and above the corotation radius. 相似文献
Polar spots are found in many Doppler images of rapidly rotating cool stars. In the past, their existence has been called into question, and it has been suggested that they could be the manifestations of NLTE (e.g. chromospheric filling in of line profiles) effects rather than real photospheric features. We assume the polar spots to be real photospheric features, and conclude that the flat-bottomed nature of the profile shape can be attributed to photospheric polar spots. The degree of truncation of the profile depends not only on spot size and strength, but also on the effective foreshortening of the polar region, a function of axial inclination.
H α is in emission on AP 149 which shows a double peak at most phases. The time-series of the profile shows an s-wave pattern as the position of these peaks changes throughout the rotation cycle. We attribute this to coronal clouds located above the stellar surface in synchronous orbit. A maximum-entropy tomogram is derived revealing four distinct emission regions located near and above the corotation radius. 相似文献
3.
I. Yu. Alekseev 《Astrophysics》2006,49(2):259-279
Three types of methods for studying the surface inhomogeneities of cool stars and the results of their use on type BY Dra,
RS CVn, FK Com, and T Tau variables are discussed. The current relevance of traditional photometric methods and the advantages
of the zonal spottedness model are pointed out. Dependences of the maximum total areas, average latitudes, and temperatures
of spots on the global parameters of the stars are given. Analogs of the solar cycle in the variations of the areas and latitudes
of starspots are examined, as well as the effects of differential rotation and active longitudes.
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Translated from Astrofizika, Vol. 49, No. 2, pp. 303–328 (May 2006). 相似文献
4.
It is well known that magnetic activity in late‐type stars increases with increasing rotation rate. Using inversion techniques akin to medical imaging, the rotationally broadened profiles from such stars can be used to reconstruct ‘Doppler images’ of the distribution of cool, dark starspots on their stellar surfaces. Interacting binaries, however, contain some of the most rapidly rotating late‐type stars known and thus provide important tests of stellar dynamo models. Furthermore, magnetic activity is thought to play a key role in their evolution, behaviour and accretion dynamics. Despite this, we know comparatively little about the magnetic activity and its influence on such binaries. In this review we summarise the concepts behind indirect imaging of these systems, and present movies of the starspot distributions on the cool stars in some interacting binaries. We conclude with a look at the future opportunities that such studies may provide. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
5.
Model results on starspots in 15 chromospherically active type RS CVn binary systems are presented. The dependences of the
parameters of the spots on the principal characteristics of the stars (spectral class, luminosity class, rotation, Rossby
number) are examined. Latitudinal drift of the spots, cycles in the spot activity, and differential rotation are found in
9 of the stars.
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Translated from Astrofizika, Vol. 48, No. 4, pp. 535–552 (November 2005). 相似文献
6.
Klaus G. Strassmeier 《Astrophysics and Space Science》1988,140(2):223-235
This paper is devoted to the effects of dark starspots on observed light curves and line profiles. A new formulation of the starspot model with multiple spots and arbitrary spot shapes is derived which allows for a numerical solution of light and colour curves and distorted line profiles simultaneously. The effects of differential rotation and the existence of a penumbra have also been considered. A parameter study demonstrates the influences of different spot parameters on the theoretical light curves and rotation profiles. The computer code is applicable for single stars as well as for eclipsing close binaries allowing for ellipticity effect and reflection effect. 相似文献
7.
Klaus G. Strassmeier 《Astronomy and Astrophysics Review》2009,17(3):251-308
Starspots are created by local magnetic fields on the surfaces of stars, just as sunspots. Their fields are strong enough
to suppress the overturning convective motion and thus block or redirect the flow of energy from the stellar interior outwards
to the surface and consequently appear as locally cool and therefore dark regions against an otherwise bright photosphere
(Biermann in Astronomische Nachrichten 264:361, 1938; Z Astrophysik 25:135, 1948). As such, starspots are observable tracers
of the yet unknown internal dynamo activity and allow a glimpse into the complex internal stellar magnetic field structure.
Starspots also enable the precise measurement of stellar rotation which is among the key ingredients for the expected internal
magnetic topology. But whether starspots are just blown-up sunspot analogs, we do not know yet. This article is an attempt
to review our current knowledge of starspots. A comparison of a white-light image of the Sun (G2V, 5 Gyr) with a Doppler image
of a young solar-like star (EK Draconis; G1.5V, age 100 Myr, rotation 10 × Ω
Sun) and with a mean-field dynamo simulation suggests that starspots can be of significantly different appearance and cannot
be explained with a scaling of the solar model, even for a star of same mass and effective temperature. Starspots, their surface
location and migration pattern, and their link with the stellar dynamo and its internal energy transport, may have far reaching
impact also for our understanding of low-mass stellar evolution and formation. Emphasis is given in this review to their importance
as activity tracers in particular in the light of more and more precise exoplanet detections around solar-like, and therefore
likely spotted, host stars. 相似文献
8.
After decades of effort, the solar activity cycle is exceptionally well characterized, but it remains poorly understood. Pioneering work at the Mount Wilson Observatory demonstrated that other Sun-like stars also show regular activity cycles, and suggested two possible relationships between the rotation rate and the length of the cycle. Neither of these relationships correctly describes the properties of the Sun, a peculiarity that demands explanation. Recent discoveries have started to shed light on this issue, suggesting that the Sun’s rotation rate and magnetic field are currently in a transitional phase that occurs in all middle-aged stars. Motivated by these developments, we identify the manifestation of this magnetic transition in the best available data on stellar cycles. We propose a reinterpretation of previously published observations to suggest that the solar cycle may be growing longer on stellar evolutionary timescales, and that the cycle might disappear sometime in the next 0.8?–?2.4 Gyr. Future tests of this hypothesis will come from ground-based activity monitoring of Kepler targets that span the magnetic transition, and from asteroseismology with the Transiting Exoplanet Survey Satellite (TESS) mission to determine precise masses and ages for bright stars with known cycles. 相似文献
9.
At present, long-term (over 30 years) multicolor photometric observations give the possibility to determine general properties
of spotted areas on late-type stars. Star-spot modeling from broadband photometric data has been carried out by Alekseev and
Gershberg since 1996 under the assumption that spots are situated in two latitudinal zones. Here we propose a new analysis
of their results for several G and K dwarf stars with high irregular activity. On these stars, EK Dra, VY Ari, V775 Her, and
V833 Tau, two spot belts exist separately and do not merge into a single equatorial active region, as occurs on cooler red-dwarf
stars. The zonal spottedness models allow us to fit simultaneously both rotational modulation and long-term variability of
stellar brightness. These models give evidence for an equatorward drift of the lower latitude boundary of the spotted region,
φ0, during the rising phase of activity, beyond any possible errors concerned with our methodology. In order to evaluate the
drift rate we introduce the concept of `effective' spot belt, whose width is independent of longitude. This permits us to
construct butterfly diagrams for stellar spots. The equatorward drift rates of the lower boundary of the spotted region D=dφlow/dt are (− 1)–(− 2) deg year−1 in the years of increasing spottedness. These values are less than the analogous solar one D≈−4 deg year−1 for the rising phase of the cycle. Thus, cyclic activity can be revealed from butterfly diagrams and derived drifts of starspots
prior to a possible detection from the spectral analysis of photometric variability. Finally, we briefly discuss a possible
explanation of high-latitude activity and surface drifts of starspots in the framework of the current state of dynamo theory. 相似文献
10.
M.S. Miesch 《Astronomische Nachrichten》2007,328(10):998-1001
In the outer envelope of the Sun and in other stars, differential rotation and meridional circulation are maintained via the redistribution of momentum and energy by convective motions. In order to properly capture such processes in a numerical model, the correct spherical geometry is essential. In this paper I review recent insights into the maintenance of mean flows in the solar interior obtained from high-resolution simulations of solar convection in rotating spherical shells. The Coriolis force induces a Reynolds stress which transports angular momentum equatorward and also yields latitudinal variations in the convective heat flux. Meridional circulations induced by baroclinicity and rotational shear further redistribute angular momentum and alter the mean stratification. This gives rise to a complex nonlinear interplay between turbulent convection, differential rotation, meridional circulation, and the mean specific entropy profile. I will describe how this drama plays out in our simulations as well as in solar and stellar convection zones. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
11.
M. Suzuki 《Solar physics》2014,289(11):4021-4029
Long-term modulation of solar differential rotation was studied with data from Mt. Wilson and our original observations during Solar Cycles 16 through 23. The results are that i) the global B-value (i.e. latitudinal gradient of differential rotation) is modulated with a period of about six or seven solar cycles, ii) the B-values of the northern and southern hemispheres are also modulated with a period similar to the global one, but iii) they show quasi-oscillatory behavior with a phase shift between them. We examined the yearly fluctuations of the B-values in every solar cycle with reference to the phase of the sunspot cycle and found that the B-values in the sunspot-minimum years show large and erratic variations, while those in the sunspot-maximum years show small fluctuations. Positive correlation between the former B-values and the latter was found. We discuss the independent long-term behavior of solar differential rotation between the northern and southern solar hemispheres and the implication for the solar dynamo. 相似文献
12.
C. Karoff T. S. Metcalfe W. J. Chaplin Y. Elsworth H. Kjeldsen T. Arentoft D. Buzasi 《Monthly notices of the Royal Astronomical Society》2009,399(2):914-923
The long-term monitoring and high photometric precision of the Kepler satellite will provide a unique opportunity to sound the stellar cycles of many solar-type stars using asteroseismology. This can be achieved by studying periodic changes in the amplitudes and frequencies of the oscillation modes observed in these stars. By comparing these measurements with conventional ground-based chromospheric activity indices, we can improve our understanding of the relationship between chromospheric changes and those taking place deep in the interior throughout the stellar activity cycle. In addition, asteroseismic measurements of the convection zone depth and differential rotation may help us determine whether stellar cycles are driven at the top or at the base of the convection zone. In this paper, we analyse the precision that will be possible using Kepler to measure stellar cycles, convection zone depths and differential rotation. Based on this analysis, we describe a strategy for selecting specific targets to be observed by the Kepler Asteroseismic Investigation for the full length of the mission, to optimize their suitability for probing stellar cycles in a wide variety of solar-type stars. 相似文献
13.
Recent observations of brightness variations on the Sun during the solar cycle have motivated us to re-examine the widely held view that cool, dark starspots, covering a significant fraction of the star, are the centers of magnetic activity on BY Dra stars. We propose that the magnetic regions are better described by a bright facular network, and that the dark areas which give rise to photometric rotational modulation are actually regions where the underlying quiet photosphere is seen. This interpretation is consistent with recent observations of late-type stars that show that bright areas covering much of the star have magnetic fields with strengths of several thousand gauss. It resolves several problems with the current model, including the size, location, and stability of the starspots required to match photometric and Doppler-imaging observations. It also has interesting observational implications for the correlation of photometric rotational modulation and long term brightness variations with other surface activity, and for the positions of magnetically active stars in the H-R diagram.Hubble Fellow. 相似文献
14.
Miyoshi Suzuki 《Solar physics》2012,278(2):257-267
We studied the solar rotation rate and its temporal change, using the sunspot data obtained during activity cycle 23 (1996 – 2006).
The equatorial rotation rate is nearly the same as in the former cycle 22, while the latitudinal gradient of differential
rotation considerably increased. Comparison of our results with others indicates the existence of a long-term periodicity
of about eight cycles in differential rotation. In addition, no significant asymmetry in differential rotation between the
northern and southern hemispheres during cycle 23 was found. The equatorial rotation rate and the latitudinal gradient of
the differential rotation in the period of cycle 23 are approximately constant, except for the initial and final phases in
the cycle. 相似文献
15.
Rapidly rotating young (T Tauri, pre-Main-Sequence, and Main-Sequence) stars as well as subgiants seem to show starspots not only at low and middle latitudes, as the Sun, but also at high latitudes and even around the poles. We consider a simple nonlinear Parker migratory dynamo model working in a thin shell in order to investigate how high latitude and polar spots may be produced for different values of the dynamo layer radius and thickness and for various rotation rates. Simple assumptions on the angular velocity gradient and helicity distribution are made according to symmetry properties and recent solar and stellar observations. A recently proposed asymptotic WKB-type approach is used to solve the dynamo problem and its drawbacks and advantages in the solar and stellar contexts are discussed. As a general result, we find that a sizable toroidal field can be produced over a much more extended latitude range than in the Sun, thus explaining in a natural way the occurrence of activity from the poles to the equator in such stars. Our approach complements that proposed by Schüssler et al. (1996) which is focused on the instability and emergence of the azimuthal flux tubes, as well as the analyses based on a dynamo working over an extended part of the stellar convective envelope (Moss, Tuominen, and Brandenburg, 1991; Moss et al., 1995). 相似文献
16.
S. V. Berdyugina 《Solar physics》2004,224(1-2):123-131
The modulation of solar activity closely follows the solar rotation period suggesting the existence of long-lived active regions
at preferred longitudes. For instance, two preferred active longitudes in both southern and northern hemispheres are found
to be persistent at the century time scale. These regions migrate with differential rotation and periodically alternate their
activity levels showing a flip-flop cycle. The pattern and behaviour of active longitudes on the Sun is similar to that on
cool, rapidly rotating stars with outer convective envelopes. This suggests that the magnetic dynamo, including non-axisymmetric
magnetic fields and flip-flop cycles, is also similar in these stars. This allows us to overview the phenomenon of stellar
magnetic activity and to study it in detail on the Sun. 相似文献
17.
Disk-integrated solar chromospheric Caii K-line (3933.68 ) fluxes have been measured almost daily at Sacramento Peak Observatory since 1977. Using observing windows selected to mimic seasonal windows for chromospheric measurements of lower Main-Sequence stars such as those observed by Mount Wilson Observatory's HK Project, we have measured the solar rotation from the modulation of the Caii K-line flux. We track the change of rotation period from the decline of cycle 21 through the maximum of cycle 22. This variation in rotation period is shown to behave as expected from the migration of active regions in latitude according to Maunder's butterfly diagram, including an abrupt change in rotation period at the transition from cycle 21 to cycle 22. These results indicate the successful detection of solar surface differential rotation from disk-integrated observations. We argue that the success of our study compared to previous investigations of the solar surface differential rotation from disk-integrated fluxes lies primarily with the choice of the length of the time-series window. Our selection of 200 days is shorter than in previous studies whose windows are typically on the order of one year. The 200-day window is long enough to permit an accurate determination of the rotation period, yet short enough to avoid complications arising from active region evolution. Thus, measurements of the variation of rotation period in lower Main-Sequence stars, especially those that appear to be correlated with long-term changes in chromospheric activity (i.e., cycles), are probably evidence for stellar surface differential rotation. 相似文献
18.
N. N. Stepanian O. A. Andryeyeva Ya. I. Zyelyk 《Bulletin of the Crimean Astrophysical Observatory》2007,103(1):48-62
The time variations in the latitudinal distribution of the rotation of active regions and coronal holes are investigated. The synoptic maps obtained from observations in the He I 1083 nm line at Kitt Peak Observatory over almost three solar cycles are used as observational data. A Fourier analysis of the time series constructed from synoptic maps has yielded the following results. The rotation of active regions differs significantly from the rotation of coronal holes in all parameters: the set of the most significant rotation periods, their latitudinal distribution, and time variations. The rotation of active regions and coronal holes is characterized by variations from cycle to cycle, a time-varying north-south asymmetry. The power spectra for consecutive cycles of solar activity differ significantly for both epochs of high activity and minima. Analysis of the total power of the spectra within four selected intervals of periods from 21 to 33 days has shown that the total power is highest in the intervals of periods 24–27 and 27–30 days. This is valid for both active regions and coronal holes. The correlation between the total powers in the above intervals of periods changes noticeably with time. Long-lived or successively appearing active regions with rotation periods in the range 24–30 days are typical of the time of a sharp decrease in the total equivalent width of active regions. This includes not only the decline time of the 11-year cycles, but also the minima between recurrent activity maxima during one cycle. A predominance of long-lived coronal holes as their total equivalent width decreases is noticeable for coronal holes with rotation periods in the interval 30–33 days. All of the above results suggest that the rotation of solar structures is determined mainly by the subphotospheric sources of specific structures, not by the rotation of the main volumes of solar plasma of the quiet Sun. 相似文献
19.
J. R. Barnes T. A. Lister R. W. Hilditch A. Collier Cameron 《Astronomische Nachrichten》2004,325(3):233-236
We present high resolution Doppler images of the short period (P = 0.362 d) contact binary AE Phe. Using least squares deconvolution, we make use of the information content of the several thousand lines in each échelle spectrum to obtain the necessary S/N and time resolution required to resolve individual starspot features. A single pair of rotationally broadened profiles (free of sidelobes due to blending) with a typical S/N of 3000 ‐ 4000 per spectrum is thus obtained. With 300 sec exposures we achieve a cadence of 350 sec which is equivalent to sampling the rotation phase every 4°. We derive images for four nights of data which reveal starspots at most latitudes on both components of the common envelope system. Individual starspots evolve significantly on very short timescales, of order one day; significantly faster than the week timescales found on active single stars and the Sun. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
20.
A. Collier Cameron 《Astrophysics and Space Science》1998,261(1-4):71-80
I review recent progress in the field of stellar surface imaging, with particular reference to advanced methods for mapping
surface-brightness inhomogeneities and the surface vector magnetic field on magnetically active late-type stars. New signal
enhancement techniques, utilising profile information from hundreds or thousands of photospheric lines simultaneously, allow
images to be derived for stars several magnitudes fainter than was previously possible. For brighter stars, the same techniques
make it possible to map features as small as two or three degrees in extent on the stellar surface. This opens up whole new
areas of research, such as the ability to use starspot tracking to study surface differential rotation patterns on single
and binary stars, and to follow the secular evolution of the magnetic field itself.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献