Spectroscopic determinations of solar rotation   总被引：2，自引：0，他引：2  

Robert Howard  J. Harvey 《Solar physics》1970,12(1):23-51

Spectral line shift data obtained from full-disk magnetograms recorded at Mt. Wilson are analyzed for differential rotation. The method of analysis is discussed and the results from the data for 1966 through 1968 are presented. The average equatorial velocity over this period is found to be 1.93 km/sec or 13.76 deg/day (sidereal). This corresponds to a sidereal period of 26.16 days. The average results are = 2.78 × 10^-6 - 3.51 × 10^-7 sin² B - 4.43 × 10^-7 sin⁴ B rad/sec, whereB is the solar latitude. This indicates a smaller decrease of angular velocity with latitude than found by earlier investigators. Variations from day to day are caused by large-scale short-lived velocity fields on the solar surface. There also appear to be secular variations.Currently at the Kitt Peak National Observatory, Tucson, Arizona.  相似文献   

Editorial     

Cornelis de Jager  Robert F. Howard  ZdenĚk švestka 《Solar physics》1993,143(1):vii-vii

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On the correlation of longitudinal and latitudinal motions of sunspots     

Peter A. Gilman  Robert Howard 《Solar physics》1984,93(1):171-175

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The ability of a field population of diatoms to discriminate between phosphate and arsenate     

R.J. Morris  M.J. McCartney  A.G. Howard  M.H. Arbab-Zavar  J.S. Davis 《Marine Chemistry》1984,14(3):259-265

Dissolved inorganic arsenic and phosphate levels present in an enclosed experimental ecosystem have been studied during the course of a natural spring diatom bloom. Whilst phosphate levels dropped rapidly to almost zero as the bloom developed, arsenic levels remained constant even when arsenate levels exceeded the dissolved phosphate. Certain diatom species (Thalassiosira spp., Chaetoceras spp. and Skeletonema costatum) therefore appear to be capable of discriminating, either by uptake or excretion, between phosphate and arsenate. The implications of such findings are discussed.  相似文献   

Implications of recent numerical calculations for the fission theory of the origin of the Moon     

Richard H. Durisen  Eugene Howard Scott 《Icarus》1984,58(2):153-158

Recent numerical simulations of fission instabilities in rotating fluid masses give results which are consistent with some requirements of the fission hypothesis for the origin of the moon.  相似文献   

Analysis and interpretation of Cassini Titan radar altimeter echoes     

Howard A. Zebker  Yonggyu Gim  Scott Hensley  Cassini Radar Team 《Icarus》2009,200(1):240-255

The Cassini spacecraft has acquired 25 radar altimeter elevation profiles along Titan's surface as of April 2008, and we have analyzed 18 of these for which there are currently reconstructed ephemeris data. Altimeter measurements were collected at spatial footprint sizes from 6-60 km along ground tracks of length 400-3600 km. The elevation profiles yield topographic information at this resolution with a statistical height accuracy of 35-50 m and kilometer-scale errors several times greater. The data exhibit significant variations in terrain, from flat regions with little topographic expression to very rugged Titanscapes. The bandwidth of the transmitted waveform admits vertical resolution of the terrain height to 35 m at each observed location on the surface. Variations in antenna pointing and changes in surface statistics cause the range-compressed radar echoes to exhibit strong systematic and time-variable biases of hundreds of meters in delay. It is necessary to correct the received echoes for these changes, and we have derived correction algorithms such that the derived echo profiles are accurate at the 100 m level for off-nadir pointing errors of 0.3° and 0.6°, for leading edge and echo centroid estimators, respectively. The leading edge of the echo yields the elevation of the highest points on the surface, which we take to be the peaks of any terrain variation. The mean value of the echo delay is more representative of the mean elevation, so that the difference of these values gives an estimate of any local mountain heights. Finding locations where these values diverge indicates higher-relief terrain. Elevation features are readily seen in the height profiles. Several of the passes show mountains of several hundred m altitude, spread over 10's or even 100's of km in spatial extent, so that slopes are very small. Large expanses of sub-100 m topography are commonplace on Titan, so it is rather smooth in many locations. Other areas exhibit more relief, although the overall observed variation in surface height on any pass is less than about 1 km. Some elevation features correspond to observed changes in brightness in Cassini infrared images, but many do not. Correspondence between the imaging SAR ground tracks and the altimeter paths is limited, so that identifying elevation changes with higher resolution SAR features is premature at present.  相似文献   

Stereoscopic Analysis of the 19 May 2007 Erupting Filament     

P. C. Liewer  E. M. De Jong  J. R. Hall  R. A. Howard  W. T. Thompson  J. L. Culhane  L. Bone  L. van Driel-Gesztelyi 《Solar physics》2009,256(1-2):57-72

A filament eruption, accompanied by a B9.5 flare, coronal dimming, and an EUV wave, was observed by the Solar TERrestrial Relations Observatory (STEREO) on 19 May 2007, beginning at about 13:00 UT. Here, we use observations from the SECCHI/EUVI telescopes and other solar observations to analyze the behavior and geometry of the filament before and during the eruption. At this time, STEREO A and B were separated by about 8.5°, sufficient to determine the three-dimensional structure of the filament using stereoscopy. The filament could be followed in SECCHI/EUVI 304 Å stereoscopic data from about 12 hours before to about 2 hours after the eruption, allowing us to determine the 3D trajectory of the erupting filament. From the 3D reconstructions of the filament and the chromospheric ribbons in the early stage of the eruption, simultaneous heating of both the rising filamentary material and the chromosphere directly below is observed, consistent with an eruption resulting from magnetic reconnection below the filament. Comparisons of the filament during eruption in 304 Å and Hα? show that when it becomes emissive in He II, it tends to disappear in Hα?, indicating that the disappearance probably results from heating or motion, not loss, of filamentary material.  相似文献   

STEREO SECCHI and S/WAVES Observations of Spacecraft Debris Caused by Micron-Size Interplanetary Dust Impacts     

St. Cyr  O. C.  Kaiser  M. L.  Meyer-Vernet  N.  Howard  R. A.  Harrison  R. A.  Bale  S. D.  Thompson  W. T.  Goetz  K.  Maksimovic  M.  Bougeret  J.-L.  Wang  D.  Crothers  S. 《Solar physics》2009,256(1-2):475-488

Early in the STEREO mission observers noted that the white-light instruments of the SECCHI suite were detecting significantly more spacecraft-related “debris” than any previously flown coronagraphic instruments. Comparison of SECCHI “debris storms” with S/WAVES indicates that almost all are coincident with the most intense transient emissions observed by the radio and plasma waves instrument. We believe the debris is endogenous (i.e., from the spacecraft thermal blanketing), and the storms appear to be caused by impacts of large interplanetary dust grains that are detected by S/WAVES. Here we report the observations, compare them to interplanetary dust distributions, and document a reminder for future spacebased coronagraphic instrument builders.

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Reconstructing the 3D Morphology of the 17 May 2008 CME     

B. E. Wood  R. A. Howard  A. Thernisien  S. P. Plunkett  D. G. Socker 《Solar physics》2009,259(1-2):163-178

We model the kinematics and three-dimensional distribution of mass in a coronal mass ejection (CME) observed on 17 May 2008, using a comprehensive analysis of STEREO images of the CME. The CME is a surprisingly fast one for solar minimum, reaching velocities of up to 1120 km?s^?1. It can be followed continuously from inception all the way out to 1 AU. We find that the appearance of the CME can be modeled reasonably well as a combination of two distinct fronts that expand outward in a self-similar fashion. The model implies that STEREO-B is struck by the weaker of these two fronts on 19 May, and the in situ instruments on STEREO-B do see a weak density and magnetic field enhancement at the expected time.  相似文献   

In Situ Observations of Solar Wind Stream Interface Evolution     

K. D. C. Simunac  L. M. Kistler  A. B. Galvin  M. A. Lee  M. A. Popecki  C. Farrugia  E. Moebius  L. M. Blush  P. Bochsler  P. Wurz  B. Klecker  R. F. Wimmer-Schweingruber  B. Thompson  J. G. Luhmann  C. T. Russell  R. A. Howard 《Solar physics》2009,259(1-2):323-344

The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45° per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few days, much less than the period of a Carrington rotation. Assuming nonevolving solar wind sources that corotate with the Sun, we calculated the expected time and longitude of arrival of stream interfaces at the Ahead observatory based on the in situ solar wind speeds measured at the Behind observatory. We find agreement to within 5° between the expected and actual arrival longitude until the spacecraft are separated by more than 20° in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25° in longitude, are observed after 20° separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and in situ measurements show that changes at the source boundary can occur on a time scale much shorter than one solar rotation. In 32 of 41 cases, the interface was observed earlier than expected at STEREO/Ahead.  相似文献