共查询到20条相似文献，搜索用时 484 毫秒
1.
An observational program at the Sacramento Peak Observatory in 1965 provided high-dispersion spectra of the solar chromosphere in several spectral regions simultaneously. These regions included various combinations of the spectral lines Hα, Hβ and H?, the D3-line of Hei, the infrared triplet of Oi, and the H- and K-lines and the infrared triplet of Caii. With the use of an image slicer the observations were made simultaneously at two heights in the solar chromosphere separated by several thousand kilometers. From these data we draw the following conclusions:
- Emission of different lines arises in the same chromospheric features. The intensity ratio of lines of different elements varies significantly from spicule to spicule. For the H- and K-lines of ionized calcium, this ratio remains constant, independent of wavelength throughout the line, overall intensity, and height in the chromosphere. Two rare-earth lines in the wing of the H-line show no spicular structure at all.
- The line-of-sight velocities of many features reverse as a function of time, although most spicules show velocities in only one direction. The simultaneous spectra at two heights show most spicules to have the same line-of-sight velocity at both. There may be an additional class of features, mostly rapidly moving, whose members have line-of-sight velocities that increase with height. These features comprise perhaps 10% of the total. Velocity changes occur simultaneously, to within 20 sec, at two heights separated by 1800 km, indicating velocities of propagation of hundreds of km/sec. The velocity field of individual features is often quite complicated; many spectral features are inclined to the direction of dispersion, implying that differential mass motions are present.
- The existence of anomalously broad H and K profiles is real. Even with high dispersion and the best seeing, such profiles are not resolved into smaller features. The central reversal in K, H and Hα appears to remain unshifted when the wings are displaced in wavelength, indicating that the reversal is non-spicular.
2.
We used the Sacramento Peak Doppler-Zeeman Analyzer to study the velocity and magnetic fields in 60 × 300 areas on the solar disk. We map the steady component of the line-of-sight velocity and longitudinal magnetic fields and compare them with the coarse Ca+ network. The collective phase behavior of the 5-min oscillations is studied in detail. We find large scale phase coherence, including waves with typical horizontal phase velocities of 100 km/sec which can be followed up to 50 000 km. The important oscillatory features are interpreted in terms of the properties of modified sound waves. We find no apparent relationship between the steady and oscillatory fields. 相似文献
3.
E. Haugen 《Solar physics》1969,9(1):88-101
The wavelength shifts of approximately 8000 absorption elements in the H-line from spectra of 66 different sunspot regions have been measured.The average velocity field in the chromosphere close to sunspots is determined. Inside 15000 km from the spot's penumbral rim the average velocity vector is directed towards the spot and downwards in the chromosphere; the angle with the horizontal direction is on the average equal to 20°. The magnitude of the average velocity vector shows a maximum of 6.8 ± 1.2 km/sec just outside the penumbral rim and decreases quickly with increasing distance from the spot. Outside 15000 km from the penumbral rim the average velocity vector is small (-0.7 km/sec) and directed nearly vertically outwards from the sun. No significant tangential component of the average velocity field is found.The deviations of the individual elements from the average velocity field are on the average larger than the value of the average velocity. The total rms deviation in the line of sight velocity is equal to 6.8 km/sec. Thus, a large number of elements, as used in this investigation, is required to give significant values of the average velocity vector.We have also observed velocities in the penumbra. The average velocity vector is here probably small and its direction uncertain. The rms deviation in the line of sight velocities observed in the penumbra is equal to 7.5 km/sec. 相似文献
4.
R. Giovanelli 《Solar physics》1975,44(2):299-314
Observations are reported of two, possibly three, distinct wave systems in the Hα chromosphere.
- Velocity films show waves propagating predominantly outwards along mottles and fibrils from as close as 2000 km to the network axis at velocities of the order of 70 km s-1. The line-of-sight component of the velocity amplitude is estimated to be typically 5 km s-1. The velocities are accompanied by propagating intensity fluctuations. The system is interpreted as one of basically Alfvén waves. Similar waves are observed propagating predominantly outwards along superpenumbral fibrils radiating from a small sunspot.
- The velocities in the chromospheric granulation undergo fluctuations of an oscillatory character but without any observable horizontal propagation. The intensities show a close correlation with the velocities, maximum intensity occurring about T/4 after maximum downward velocity. The period is variable across the surface (2.5 min upwards). The intensity-velocity correlation is characteristic of a standing compressional wave.
- Intensity cinefilms at Hα line centre show in places a horizontal drift of the chromospheric granulation pattern at about 12 km s-1 without any accompanying vertical velocity fluctuations. It is not known whether this is due to a gas stream at sonic velocities, or to a horizontally propagating sound wave.
5.
An X2.3 class flare was reported on 10 April 2001 in AR 9415. A halo coronal mass ejection (CME) was associated with this flare. The Coronal Diagnostic Spectrometer (CDS) on board the Solar and Heliospheric Observatory (SOHO), which was running in its daily synoptic mode, recorded a very high-velocity ejection of plasma associated with this activity. The spatial scanning and spectral capabilities of CDS allow the measurement of both transverse and line-of-sight velocities. Components of the plasma, as seen in emission from Ov at around 2.5×105 K, reached transverse velocities in excess of 800 km s–1. The nature of the spectral line profiles suggests that a rotational motion of ±350 km s–1 was superimposed upon the general outward expansion of approximately 150 km s–1. The ejection detected using CDS was found to have a constant acceleration and is thought to be a spray of plasma with a helical structure driven by the magnetic topology. 相似文献
6.
Profiles of weak Fraunhofer lines have been recorded photoelectrically in both the faculae and the undisturbed photosphere. The entrance slit of the double-pass spectrograph corresponded to 1 × 20 on the solar disk. Turbulent velocities were found by comparing half-widths of the observed profiles with those of model calculations. These latter were carried out with aid of an electronic computer for the Bilderberg Continuum Atmosphere (BCA) under the assumption of true absorption and depth independent turbulent velocities. Line-formation levels were derived from the contribution curves computed by the method of weighting functions. For the undisturbed photosphere a turbulent velocity of about 2.6 km/s was found with no appreciable increase with the depth. In facular filaments all lines formed above = 0.1 showed smaller turbulence velocities, the velocity differences being in the range between 0.2 and 0.6 km/s (see Table II). 相似文献
7.
M. N. Pasechnik 《Kinematics and Physics of Celestial Bodies》2014,30(4):161-172
The results of analyzing variations in the line-of-sight (LOS) velocities in the solar loop at photospheric and chromospheric levels in the region of emerging magnetic flux for the evolving active region NOAA 11024 are reported. The analysis combines the data of multiwave spectropolarimetric observations that were carried out on July 4, 2009, (Tenerife, Spain) using THEMIS solar telescope and the data obtained with GOES, SOHO, and STEREO cosmic satellites. A complex sequence of active events has been studied: formation of the Ellerman bomb, B1 X-ray microflare, and four chromospheric surges that were formed as a result of magnetic reconnection caused by new emerging magnetic flux. The Ellerman bomb was formed in the vicinity of a growing pore. Variations in the velocity V LOS of the EB had an oscillation character for chromosphere and photosphere. Before the microflare, the average velocities of the upward and downward plasma fluxes in one leg of the magnetic loop were nearly the same—26 km/s. During the microflare, the velocity V LOS of the ascending and descending flows increased up to ?33 and 50 km/s, respectively. Variations in line-of-sight velocity of a plasma in the second leg of the magnetic loop correlated well with variations of V LOS in the region of microflare, but they occurred 1.5 minutes later. During the time of observations, four chromospheric ejections of matter were formed and three of them occurred in the region of Ellerman’s bomb formation. Sharp variations in the soft X-ray intensity occurred during these ejections. At photospheric level, variations in the line-of-sight velocity of plasma in the legs of the loop occurred in the opposite direction. In the region of the first leg, velocity V LOS diminished from ?1.8 to ?0.4 km/s, while the velocity increased from ?0.6 to ?2.6 km/s in the region of the second leg. 相似文献
8.
The Solar Ultraviolet Measurements of Emitted Radiation instrument (SUMER) observations show high Doppler shifts and temporal variations in profiles of ultraviolet lines from low temperature gas in the corona above the active region NOAA 7974. The profiles indicate 100 km s-1 flows coming from an almost stationary source that appears bright in the lines of N III and Si III. The variations in line-of-sight velocities and intensities suggest small knots of cooling plasma emanating from a small region high in the corona. A few arc sec sunward of the region where the cool flows are seen is an elongated region of enhanced higher temperature, low velocity Ne VI and Mg VI line emission. 相似文献
9.
Meteoroids that orbit the Sun encounter the Earth with speeds between 11 and 74 km/sec. However, the distribution of the velocities of meteoroids between these limits is not well known. The uncertainty is caused by the difficulty in measuring the true flux of meteors at the extrema of the velocity distribution. Whilst the most comprehensive measurements of meteor flux are those obtained using radio techniques, meteors with speeds > 50 km/sec occur at heights where the effects of initial radius of the trail and diffusion significantly reduce the radio reflection from the trails; on the other hand the high dependence of the collisional ionization probability on velocity (to the power 3.5) significantly inhibits the detection of meteors with speeds < 20 km/sec. Recent developments in meteor radar systems are now making it possible to measure the velocity of meteors at the extrema of the distribution. For meteoroids ablating at heights between 100 and 120 km the speed of entry can be measured at 2 and 6 MHz using a radar with a 1 km diameter array located near Adelaide; these observations will commence early in 1995. In the meantime a 54 MHz MST radar is being operated at a pulse repetition frequency of 1024 Hz to search for the presence of interstellar (speed > 74 km/sec) meteors. Both these radars exploit the phase information available prior to the closest-approach (to) point. 相似文献
10.
We report a catalog of 168 galaxy triplets with line-of-sight velocities V LG < 3500 km/s identified using a percolation criterion, which takes individual properties of galaxies into account. The catalog contains the line-of-sight velocities, K-band magnitudes, and morphological types of galaxies. Our sample of galaxy triplets is characterized by the median values of the line-of-sight velocity dispersion, projected harmonic radius, and crossing time of 40 km/s, 155 kpc, and 3 Gyr, respectively. The median projectedmass and K-band luminosity of our triplets are equal to 5 × 1011 M ⊙ and 15M ⊙/L ⊙, respectively, with the uncertainty of these parameters due mostly to the errors of radial-velocity measurements. The basic properties of triple systems in the Local Supercluster are compared to those of more distant isolated triplets from the KTG and KTS samples. The fraction of triplet members among all galaxies is found be more than 5%. 相似文献
11.
Anne B. Underhill 《Astrophysics and Space Science》1969,3(1):109-116
Wolf-Rayet stars are defined, a summary is given of the properties of Wolf-Rayet stars, and a qualitative model of a Wolf-Rayet star is sketched. It is incontrovertible that Wolf-Rayet stars are losing mass, a typical rate of mass loss being near 10–5
M
per year. The outward directed velocity of the expanding shell has been estimated for 10 stars. The largest value found is 2500 km/sec; most values lie between 1000 and 1500 km/sec. Two outstanding problems are to understand how the observed high velocities are generated and to demonstrate quantitatively the effect of these velocities on the observed spectrum. Five questions raised by the fact that mass loss is observed to take place from Wolf-rayet stars are discussed briefly in Section 5.Presented at the Trieste Colloquium on Mass Loss from Stars, September 12–16, 1968. 相似文献
12.
Ray A. Williamson 《Astrophysics and Space Science》1970,6(1):45-59
A photographic Fabry-Pérot interferometer was built for the University of Maryland's 20-in. telescope for the study of the radial velocities of diffuse emission nebulae. Observations of S101, S112, IC5146, NGC7380, NGC281, and IC1795 were made and radial velocities at many points within each nebula were determined with an estimated error of ±3 km/sec. Average heliocentric radial velocities were obtained for each nebula and they agree well with those found by other observers.For S112 and IC5146, a systematic difference of 6–8 km/sec in the radial velocities between the east and west sides of the nebulae was observed. This phenomenon is attributed to the braking effect of cold gas which appears to be associated with the western side of both nebulae.Ring half-widths were obtained for S112, IC5146 and NGC281, and found to be consistent with expansion velocities of 5 km/sec or less. For IC5146 the average Doppler temperature is only 5500±1000 K, which indicates an even lower electron temperature. 相似文献
13.
A quiescent prominence has been observed with the MSDP spectrograph at the Pic du Midi Observatory. H profiles are obtained simultaneously in a 2D field, allowing a statistical analysis. The standard deviations of Doppler shifts and line widths are investigated as functions of the line intensity. The observations are compared with numerical simulations assuming that the prominence is made of identical threads, the velocity of which is distributed according to gaussian functions. The processing of simulations is very close to the processing of observations. The mixing by seeing effects and the transfer of radiation across several threads along the line of sight are considered. The results are consistent with the values derived by Engvold et al. (1989) and Zirker and Koutchmy (1989, 1990, 1991).The best fits are obtained with the following conditions. The temperature is 8500 K. In the middle range of intensities, each pixel results typically from the mixing of 6 velocity threads, the optical thickness of which is roughly 0.2 at H center, and the geometrical thickness larger than 1000 km. It is likely that the velocity threads have larger sizes than the density threads. The fit of the results is improved by taking into account a slight scatter of source functions throughout the prominence.In the central parts of the prominence, the fit is obtained by assuming that the line-of-sight velocities of the threads have a gaussian probability function (standard deviation 7 km s–1).In the edges, we suggest larger scatter of velocities, and two combined dispersions. The velocity threads observed along a given line of sight are supposed to have neighbouring velocities (dispersion 7 km s–1) around a mean value taken at random inside another distribution function (dispersion 7 km s–1). 相似文献
14.
The shape parameters of a number of selected ultraviolet lines in BUSS-spectra of the Beta Cephei stars Peg and Cep have been analyzed to determine the principal parameters of the atmospheric velocity field. We find for both stars a fairly high value (5 km s–1) for the microturbulent line-of-sight velocity component, which confirms an earlier result based on lower resolution UV spectra. Macroturbulent and rotational velocities are virtually zero in the atmosphere of Peg; for Cep we findv
rotsini=40 km s–1.On leave from Akita University, Akita, Japan. 相似文献
15.
Fokker (1967) has raised the question of whether the optical and radio homologies of flares are correlated. Two 2b flares occurring nearly 54 h apart (July 9 and 12, 1968) were observed at 29 wavelengths from H+4.00 Å to H–4.26 Å and at 10-cm radio. Adjacent pictures were spaced 0.295 Å and 2 sec apart. The time resolution of the radio traces was about 10 sec. Detailed comparison of the pictures showed near-perfect similarities in the two events. These similarities included flare shape, filament agitation, rising arch formation and surges with line-of-sight velocities nearly 200 km/ sec observed. Comparion of the microwave radio flux traces showed detailed similarities in the shapes and simultaneity of at least eight features.Research supported in part by the Atmospheric Sciences Section, National Science Foundation, NSF Grant GA-4184, while at Harvey Mudd College, Claremont, Calif. 相似文献
16.
J. M. Beckers 《Solar physics》1968,3(2):258-268
Modifications to a Zeiss 1/4 Å filter are described which allow high spatial resolution observations of the line-of-sight velocities and magnetic fields in the photosphere and in sunspots. First results show: (1) the granular velocity field to be very strong; differences in upward motions in the granules and downward motions in between are as much as 6 km/sec; (2) the Evershed effect in sunspots to originate primarily in the dark regions between bright penumbral filaments. 相似文献
17.
Richard C. Canfield 《Solar physics》1976,50(2):239-254
Previous observations of spatially-resolved vertical velocity variations in ten lines of Fe i spanning the height range 0 h 1000 km are re-analyzed using velocity weighting functions. The amplitudes and scale heights of granular and oscillatory velocities are determined, as well as those of the remaining unresolved velocities. I find that the optimal representation of the amplitude of the outward-decreasing granular velocities is an exponentially decreasing function of height, with a scale height of 150 km and a velocity at zero height of 1.27 km s–1. The optimal representation of the same quantities for oscillatory velocities is an exponential increase with height, with a scale height of 1100 km and a velocity at zero height of 0.35 km s–1. The remaining unresolved velocities decrease with height, with a scale height of 380 km and a velocity at zero height of 2.3 km s–1. 相似文献
18.
The catalogue of protoplanetary nebulae by Vickers et al. has been supplemented with the line-of-sight velocities and proper motions of their central stars from the literature. Based on an exponential density distribution, we have estimated the vertical scale height from objects with an age less than 3 Gyr belonging to the Galactic thin disk (luminosities higher than 5000 L ⊙) to be h = 146 ± 15 pc, while from a sample of older objects (luminosities lower than 5000 L ⊙) it is h = 568 ± 42 pc. We have produced a list of 147 nebulae in which there are only the line-of-sight velocities for 55 nebulae, only the proper motions for 25 nebulae, and both line-of-sight velocities and proper motions for 67 nebulae. Based on this kinematic sample, we have estimated the Galactic rotation parameters and the residual velocity dispersions of protoplanetary nebulae as a function of their age. We have established that there is a good correlation between the kinematic properties of nebulae and their separation in luminosity proposed by Vickers. Most of the nebulae are shown to be involved in the Galactic rotation, with the circular rotation velocity at the solar distance being V 0 = 227 ± 23 km s?1. The following principal semiaxes of the residual velocity dispersion ellipsoid have been found: (σ1, σ2, σ3) = (47, 41, 29) km s?1 from a sample of young protoplanetary nebulae (with luminosities higher than 5000 L ⊙), (σ1, σ2, σ3) = (50, 38, 28) km s?1 from a sample of older protoplanetary nebulae (with luminosities of 4000 L ⊙ or 3500 L ⊙), and (σ1, σ2, σ3) = (91, 49, 36) km s?1 from a sample of halo nebulae (with luminosities of 1700 L ⊙). 相似文献
19.
Published data on gas systems of different velocities in the galaxy NGC 1275 are examined. One of the systems is associated with NGC 1275 (low-velocity system — LV); the other is approaching it at a velocity of 3000 km/sec (high-velocity system — HV). Many of the collected results obtained from spectra and from direct images in the ultraviolet, optical, red, and infrared indicate interaction of these systems. The interaction is exhibited in the same shape and spatial distribution of the gas filaments in both systems, in the elongation of some of them toward the nucleus of the galaxy, and in the increase in brightness of the HV gas near some of the clusters of young stars of the LV system. Gas of the HV system is observed at a distance of O.5 (170 pc) from the nucleus of the galaxy, while intermediate-velocity gas (IV — 600–1520 km/sec relative to the velocity of NGC 1275) is detected at distances less than 7 (2.5 kpc). We presume that the rare cases of the detection of IV gas are related to the use of Ha observations primarily: at the velocities of 600–900 km/sec, the Ha line of the IV gas blends with the [NII] 6584Å line of the LV gas.Translated fromAstrofizika, Vol. 39, No. 4, pp. 567–584, November, 1996. 相似文献
20.
Ian Elliott 《Solar physics》1969,6(1):28-40
The temporal characteristics of the chromospheric velocity field in a quiet region are studied by means of a carefully guided sequence of 215 H spectra of the disk centre lasting 54 min. The Doppler shifts of each frame at = 0.4 Å are measured and the velocity history of each position on the sun is reconstructed. The velocity power spectrum is found for each of 256 points along the total slit length of 280000 km.A steady downward velocity is associated with places where the amplitude of the fluctuating velocity is high. The average velocity power spectrum exhibits three main features: (1) A peak at 287 sec, (2) A group of high frequency peaks in the range 150–210 sec, and (3) A low frequency peak with a period of 900 sec.The relationship of these features to the Ca K network is discussed.Member of the High Altitude Observatory Solar Project at Sacramento Peak, on leave from Dunsink Observatory, Ireland. 相似文献