共查询到20条相似文献，搜索用时 31 毫秒
1.
W. J. Chaplin J. Christensen-Dalsgaard Y. Elsworth R. Howe G. R. Isaak R. M. Larsen R. New J. Schou M. J. Thompson S. Tomczyk 《Monthly notices of the Royal Astronomical Society》1999,308(2):405-414
Determination of the rotation of the solar core requires very accurate data on splittings for the low-degree modes which penetrate to the core, as well as for modes of higher degree to suppress the contributions from the rest of the Sun to the splittings of the low-degree modes. Here we combine low-degree data based on 32 months of observations with the BiSON network and data from the LOWL instrument. The data are analysed with a technique that specifically aims at obtaining an inference of rotation that is localized to the core. Our analysis provides what we believe is the most stringent constraint to date on the rotation of the deep solar interior. 相似文献
2.
S. Turck-Chièze S. Basu A. S. Brun J. Christensen-Dalsgaard A. Eff-Darwich I. Lopes F. Pérez Hernández G. Berthomieu J. Provost R. K. Ulrich F. Baudin P. Boumier J. Charra A. H. Gabriel R. A. Garcia G. Grec C. Renaud J. M. Robillot T. Roca Cortés 《Solar physics》1997,175(2):247-265
After 8 months of nearly continuous measurements the GOLF instrument, aboard SOHO, has detected acoustic mode frequencies
of more than 100 modes, extending from 1.4 mHz to 4.9 mHz. In this paper, we compare these results with the best available
predictions coming from solar models. To verify the quality of the data, we examine the asymptotic seismic parameters; this
confirms the improvements achieved in solar models during the last decade.
Using the GOLF set of frequencies for l=0, 1, 2, 3 combined with the LOWL second year data set for l > 3 we then carry out
inversions to infer properties of the solar core.
This largely confirms the previous results down to around 0.1 R⊙, while there remain differences, even closer to the centre,
where the present study shows an extreme sensitivity of the inversion results to the values of the frequencies. We finally
consider physical processes which may influence directly or indirectly the solar core structure. 相似文献
3.
A. M. Broomhall W. J. Chaplin Y. Elsworth R. New 《Monthly notices of the Royal Astronomical Society》2009,397(2):793-801
Birmingham Solar Oscillations Network (BiSON) instruments use resonant scattering spectrometers to make unresolved Doppler velocity observations of the Sun. Unresolved measurements are not homogenous across the solar disc and so the observed data do not represent a uniform average over the entire surface. The influence on the inhomogeneity of the solar rotation and limb darkening has been considered previously and is well understood. Here, we consider a further effect that originates from the instrumentation itself. The intensity of light observed from a particular region on the solar disc is dependent on the distance between that region on the image of the solar disc formed in the instrument and the detector. The majority of BiSON instruments have two detectors positioned on opposite sides of the image of the solar disc and the observations made by each detector are weighted towards differing regions of the disc. Therefore, the visibility and amplitudes of the solar oscillations and the realization of the solar noise observed by each detector will differ. We find that the modelled bias is sensitive to many different parameters such as the width of solar absorption lines, the strength of the magnetic field in the resonant scattering spectrometer, the orientation of the Sun's rotation axis, the size of the image observed by the instrument and the optical depth in the vapour cell. We find that the modelled results best match the observations when the optical depth at the centre of the vapour cell is 0.55. The inhomogeneous weighting means that a 'velocity offset' is introduced into unresolved Doppler velocity observations of the Sun, which varies with time, and so has an impact on the long-term stability of the observations. 相似文献
4.
GOLF (Global Oscillations at Low Frequencies) is an instrument to study the line-of-sight velocity of the solar photosphere, to be flown on the SOHO satellite in 1995. It uses a sodium vapour cell in resonance scattering mode, in order to measure the absolute Doppler shift of the solar sodium absorption lines. We detail laboratory tests to determine the performances of the cell built for the experiment. The results are in good agreement with numerical simulations of the resonance processes. As a final result, we can conclude that the level of performances required for the flight instrument will be obtained. 相似文献
5.
A Stokes polarimeter has been built at the High Altitude Observatory to obtain line profiles in both linear and circular polarization in solar spectral lines. These measurements are interpreted using the theory of radiative transfer in the presence of a magnetic field to obtain vector magnetic fields on the solar disk and using the theory of resonance scattering and the Hanle effect to obtain vector magnetic fields in prominences. The polarimeter operates on the Sacramento Peak Observatory 40 cm coronagraph. It is an extensively modified and improved version of an earlier instrument.Polarization modulation is achieved by two KD*P Pockels cells at the coronagraph prime focus and demodulation is by a microprocessor. The instrument control and data handling is done by a minicomputer. Silicon photodiode 128 element line array detectors have replaced the two photomultipliers used on the earlier instrument. This gives a speed increase of a factor of 50.A polarization scrambler provides a chop to a reference beam of unpolarized light by time scrambling the polarization of the solar beam. This device improves sensitivity to polarizations less than 0.01%. The polarization measurements are photon noise limited in most cases. This noise is 0.1% for a typical three second observation which is about one gauss on the longitudinal field and 10 gauss on the transverse field.The National Center for Atmospheric Research is sponsored by The National Science Foundation. 相似文献
6.
Shanmugaraju A. Umapathy S. Balasubramanian V. Selvanayagam A.J. Manoharan P.K. 《Solar physics》1999,188(1):155-162
A new digital radio spectrograph, the Madurai Solar Radio Spectrograph (MSRS), has been constructed at Madurai Kamaraj University, Madurai, India, and is being operated at the Radio Astronomy Centre, Ooty in southern India to observe solar bursts in the frequency range 30–80 MHz. The operation of the new instrument is briefly described. Observations of solar bursts by this instrument and the results from the preliminary analysis are presented. 相似文献
7.
Harrison P. Jones Thomas L. Duvall Jr. John W. Harvey Charles T. Mahaffey Jan D. Schwitters Jorge E. Simmons 《Solar physics》1992,139(2):211-232
The NASA/NSO Spectromagnetograph is a new focal plane instrument for the National Solar Observatory/Kitt Peak Vacuum Telescope which features real-time digital analysis of long-slit spectra formed on a two-dimensional CCD detector. The instrument is placed at an exit port of a Littrow spectrograph and uses an existing modulator of circular polarization. The new instrument replaces the 512-channel Diode Array Magnetograph first used in 1973. Commercial video processing boards are used to digitize the spectral images at video rates and to separate, accumulate, and buffer the spectra in the two polarization states. An attached processor removes fixed-pattern bias and gain from the spectra in cadence with spatial scanning of the image across the entrance slit. The data control computer performs position and width analysis of the line profiles as they are acquired and records line-of-sight magnetic field, Doppler shift, and other computed parameters. The observer controls the instrument through windowed processes on a data control console using a keyboard and mouse. Early observations made with the spectromagnetograph are presented and plans for future development are discussed.The National Solar Observatory is a Division of the National Optical Astronomy Observatories which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 相似文献
8.
The Solar–Stellar Irradiance Comparison Experiment {II (SOLSTICE {II), aboard the Solar Radiation and Climate Experiment (SORCE)
spacecraft, consists of a pair of identical scanning grating monochromators, which have the capability to observe both solar
spectral irradiance and stellar spectral irradiance using a single optical system. The SOLSTICE science objectives are to
measure solar spectral irradiance from 115 to 320 nm with a spectral resolution of 1 nm, a cadence of 6 h, and an accuracy
of 5%, to determine its variability with a long-term relative accuracy of 0.5% per year during a 5-year nominal mission, and
to determine the ratio of solar irradiance to that of an ensemble of bright B and A stars to an accuracy of 2%. Those objectives
are met by calibrating instrument radiometric sensitivity before launch using the Synchrotron Ultraviolet Radiation Facility
at the National Institute for Standards and Technology in Gaithersburg, Maryland. During orbital operations irradiance measurements
from an ensemble of bright, stable, main-sequence B and A stars are used to track instrument sensitivity. SORCE was launched
on 25 January 2003. After spacecraft and instrument check out, SOLSTICE {II first observed a series of three stars to establish
an on-orbit performance baseline. Since 6 March 2003, both instruments have been making daily measurements of both the Sun
and stars. This paper describes the pre-flight and in-flight calibration and characterization measurements that are required
to achieve the SOLSTICE science objectives and compares early SOLSTICE{II measurements of both solar and stellar irradiance
with those obtained by SOLSTICE {I on the Upper Atmosphere Research Satellite. 相似文献
9.
MEASURING DOPPLER AND MAGNETIC FIELDS SIMULTANEOUSLY 总被引：1，自引：0，他引：1
A compact and inexpensive version of the magneto-optical filter, developed in Rome during the 1970s, has attained the capability to measure all the Stokes' parameters on the full solar disk. Without the help of moving parts, each Stokes' image is taken simultaneously with a companion Doppler image. The overall instrument is about 15 × 15 × 50 cm in size (telescope included). The working principle of the instrument is described first, then samples of its present applications are given. In this paper we address, for the first time, questions relating to the MOF lifetime and their implications on space applications. 相似文献
10.
J. O. Stenflo D. Dravins N. Wihlborg A. Bruns V. K. Prokof'ev I. A. Zhitnik H. Biverot L. Stenmark 《Solar physics》1980,66(1):13-19
An instrument designed to record polarization in the region 120–150 nm of the solar spectrum was launched on the satellite Intercosmos-16, July 27, 1976. The aim was to search for resonance-line polarization that is caused by coherent scattering. Oblique reflections at gold- and aluminium-coated mirrors in the instrument were used to analyze the polarization. The average polarization of the L solar limb was found to be less than 1%. It is indicated how future improved VUV polarization measurements may be a diagnostic tool for chromospheric and coronal magnetic fields and for the three-dimensional geometry of the emitting structures.On leave from Lund Observatory, S-22224 Lund, Sweden.The National Center for Atmospheric Research is sponsored by the National Science Foundation. 相似文献
11.
Recently a new version of a sodium double-band magneto-optical filter has been built in order to provide simultaneous Doppler and magnetograms using the same optical path (Cacciani, Moretti, and Rodgers, 1997; Cacciani et al., 1988, 1994). Two observing stations based on this instrument are being installed as part of the French network IRIS. One is already operational in Apple Valley, California, and the other one will be delivered shortly to Tashkent, Uzbekistan. The performance of the instrument is such as to detect the l = 0 mode of solar oscillations from resolved images with a signal-to-noise ratio that has never been achieved before (Cacciani and Moretti, 1994). The magnetic and velocity signals are corrected for the changes that occur in the solar D-line profile in active versus non-active regions. This kind of analysis will be performed by our group in conjunction with parallel analysis of GOLF and IRIS integrated data which use the same sodium lines. 相似文献
12.
GOLF (Global Oscillations at Low Frequencies) is an instrument to study the line-of-sight velocity of the solar photosphere, to be flown on the SOHO satellite in 1995. It uses a sodium vapour cell in resonance scattering mode, in order to measure the absolute Doppler shift of the solar sodium absorption lines. We have developed a model of the resonance cell performance. We describe here the main characteristics of the model, and report the most important results concerning the performance of the cell and its dependance on temperature. 相似文献
13.
S. Gburek M. Siarkowski A. Kepa J. Sylwester M. Kowalinski J. Bakala P. Podgorski Z. Kordylewski S. Plocieniak B. Sylwester W. Trzebinski S. Kuzin 《Solar System Research》2011,45(2):182-187
Solar Photometer in X-rays (SphinX) is an instrument designed to observe the Sun in X-rays in the energy range 0.85–15.00 keV. SphinX is incorporated within the Russian TESIS X and EUV telescope complex aboard the CORONAS-Photon satellite which was launched on January 30, 2009 at 13:30 UT from the Plesetsk Cosmodrome, northern Russia. Since February, 2009 SphinX has been measuring solar X-ray radiation nearly continuously. The principle of SphinX operation and the content of the instrument data archives is studied. Issues related to dissemination of SphinX calibration, data, repository mirrors locations, types of data and metadata are discussed. Variability of soft X-ray solar flux is studied using data collected by SphinX over entire mission duration. 相似文献
14.
R. M. MacQueen A. Csoeke-Poeckh E. Hildner L. House R. Reynolds A. Stanger H. Tepoel W. Wagner 《Solar physics》1980,65(1):91-107
The High Altitude Observatory Coronagraph/Polarimeter, to be flown on the National Aeronautics and Space Administration's Solar Maximum Mission satellite, is designed to produce images of the solar corona in seven wavelength bands in the visible spectral range. The spectral bands have been chosen to specifically exclude or include chromospheric spectral lines, so as to allow discrimination between ejecta at high (coronal) and low (chromospheric) temperatures, respectively. In addition, the instrument features spectral filters designed to permit an accurate color separation of the F and K coronal components, and a narrow band (5.5 Å) filter to observe the radiance and polarization of the Fe xiv 5303 Å line. The effective system resolution is better than 10 arc sec and the instrument images a selected quadrant (or smaller field) on an SEC vidicon detector. The total height range that may be recorded encompasses 1.6 to more than 6.0R
(from Sun center). The instrument is pointed independently of the SMM spacecraft, and its functions are controlled through the use of a program resident within the onboard spacecraft computer. Major experimental goals include: (a) Observation of the role of the corona in the flare process and of the ejecta from the flare site and the overlying corona; (b) the study of the direction of magnetic fields in stable coronal forms, and, perhaps, ejecta; and (c) examination of the evolution of the solar corona near the period of solar maximum activity.The National Center for Atmospheric Research is sponsored by the National Science Foundation. 相似文献
15.
Phillips K.J.H. Read P.D. Gallagher P.T. Keenan F.P. Rudawy P. Rompolt B. Berlicki A. Buczylko A. Diego F. Barnsley R. Smartt R.N. Pasachoff J.M. Babcock B.A. 《Solar physics》2000,193(1-2):259-271
The Solar Eclipse Coronal Imaging System (SECIS) is an instrument designed to search for short-period modulations in the solar corona seen either during a total eclipse or with a coronagraph. The CCD cameras used in SECIS have the capability of imaging the corona at a rate of up to 70 frames a second, with the intensities in each pixel digitised in 12-bit levels. The data are captured and stored on a modified PC. With suitable optics it is thus possible to search for fast changes or short-period wave motions in the corona that will have important implications for the coronal heating mechanism. The equipment has been successfully tested using the Evans Solar Facility coronagraph at National Solar Observatory/Sacramento Peak and during the 11 August 1999 eclipse at a site in north-eastern Bulgaria. The instrument is described and preliminary results are outlined. 相似文献
16.
The recently upgraded system of the ground-based Global Oscillation Network Group (GONG) network of helioseismic observatories
has started to provide higher-resolution solar oscillation measurements suitable for local helioseismic studies. Selecting
simultaneously observed regions on the Sun by both GONG and the space-borne Michelson Doppler Imager (MDI) instrument on board
the Solar and Heliospheric Observatory (SOHO), we perform a comparative analysis of time-distance measurements focussing on
the noise properties. 相似文献
17.
The ground based full disk velocity Doppler measurements used in helioseismology suffer from an atmospheric noise component when the sky transparency is not perfect. It is due to the non uniform integration of the line of sight component of the solar rotation produced by the differential atmospheric extinction across the direction of the solar equator. A simple two-channel differential photometer is proposed for measuring this differential extinction. The first laboratory tests of this instrument show that it has the capability of performing the required correction without adding a significant level of new instrumental noise contribution.
相似文献18.
In this paper a procedure to calibrate dopplergrams is presented. This procedure is instrument independent and is based on the main topological characteristics of solar rotation. It is reliable in those regions on the solar disk where the sensitivity can be considered linear in the east-west direction (that is, out to 0.75 solar radius for most instruments) and, in principle, can be applied to all dopplergrams with medium spatial resolution (typically 8 arc sec pixel–1). The aim of this calibration is to correct any variation of the sensitivity to the velocity signal caused by instrumental changes. The procedure is currently applied to data obtained at the Solar Observatory at Kanzelhöhe (Austria) with a sodium magneto-optical filter. The procedure, applied to a one-day run, shows how the low-degree five-min oscillations are recovered from the raw integrated Doppler signal over the whole CCD. 相似文献
19.
We suggest a solution to an important problem in observational helioseismology of the separation of lines of solar acoustic (p) modes of low angular degree in oscillation power spectra by constructing optimal masks for Doppler images of the Sun. Accurate measurements of oscillation frequencies of low-degree modes are essential for the determination of the structure and rotation of the solar core. However, these measurements for a particular mode are often affected by leakage of other p-modes arising when the Doppler images are projected on to spherical harmonic masks. The leakage results in overlapping peaks corresponding to different oscillation modes in the power spectra. In this Letter, we present a method for calculating optimal masks for a given (target) mode by minimizing the signals of other modes appearing in its vicinity. We apply this method to time series of 2 yr obtained from the Michelson Doppler Imager instrument on board the Solar and Heliospheric Observatory space mission and demonstrate its ability to reduce efficiently the mode leakage. 相似文献
20.
N. I. Kobanov 《Experimental Astronomy》1994,5(3-4):301-313
A variant to implement a spacecraft (SC) spatial attitude system with respect to the Sun is discussed. The sunward direction and the solar rotation axis are used as reference points. The system is based on measuring spectral line Doppler shift by scanning the solar image along the limb and is self-adjusting for relative spectral line shifts and instrument band shifts. The first harmonic of the signal serves as a basis for accurate adjustment of filter band. The second harmonic phase is used to measure the spacecraft attitude. The application of this method holds the greatest promise when the SO is stabilized by the sunward spinning because this ensures continuous monitoring of the spacecraft attitude.In addition, the method provides information on the precise coordinates of solar surface details during space-borne observations. 相似文献