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1.
Abstract— Recent estimates of the current rate of meteorite falls have been derived from camera network observations and from the statistics of the recovery of small fragments in Roosevelt County, New Mexico. The results are discordant. The integrated sky coverage for the camera data is an order of magnitude greater than the long exposure over small areas in New Mexico, yet the number of inferred events is comparable. We examine potential problems and find no effects other than random ones to bias the camera data. New data on the total number of suitable fireballs indicate that the flux from the camera network is already close to the upper limit imposed by the count of over 700 fireballs. By contrast, the calibration of the decay time for small fragments in New Mexico appears insecure and could account for a factor-of-three discrepancy. The large area of a typical strewn field relative to the small search areas is also a serious problem that remains uncalibrated. There are problems with the application of either the camera results or the New Mexico data to the statistics of recoveries in Antarctica since the Antarctic search areas are not free from the strewn-field problem. Since there is no evidence for a substantial change in the infall rate in intervals less than the ages of the collecting surfaces, we believe the camera network flux data remain the best estimate for the arrival rate of small meteorites on Earth.  相似文献   

2.
New paleovegetation and paleoclimatic reconstructions from the Sierra Madre Occidental (SMO) in northwestern Mexico are presented. This work involves climate and biome reconstruction using Plant Functional Types (PFT) assigned to pollen taxa. We used fossil pollen data from four Holocene peat bogs located at different altitudes (1500‑2000 m) at the border region of Sonora and Chihuahua at around 28° N latitude (Ortega-Rosas, C.I. 2003. Palinología de la Ciénega de Camilo: datos para la historia de la vegetación y el clima del Holoceno medio y superior en el NW de la Sierra Madre Occidental, Sonora, Mexico. Master Thesis, Universidad Nacional Autónoma de México, México D.F.; Ortega-Rosas, C.I., Peñalba, M.C., Guiot, J. Holocene altitudinal shifts in vegetation belts and environmental changes in the Sierra Madre Occidental, Northwestern Mexico. Submitted for publication of Palaeobotany and Palynology). The closest modern pollen data come from pollen analysis across an altitudinal transect from the Sonoran Desert towards the highlands of the temperate SMO at the same latitude (Ortega-Rosas, C.I. 2003. Palinología de la Ciénega de Camilo: datos para la historia de la vegetación y el clima del Holoceno medio y superior en el NW de la Sierra Madre Occidental, Sonora, Mexico. Master Thesis, Universidad Nacional Autónoma de México, México D.F.). An additional modern pollen dataset of 400 sites across NW Mexico and the SW United States was compiled from different sources (Davis, O.K., 1995. Climate and vegetation pattern in surface samples from arid western U.S.A.: application to Holocene climatic reconstruction. Palynology 19, 95–119, North American Pollen Database, Latin-American Pollen Database, personal data, and different scientific papers). For the biomization method (Prentice, I.C., Guiot, J., Huntley, B., Jolly, D., Cheddadi, R., 1996. Reconstructing biomes from paleoecological data: a general method and its application to European pollen data at 0 and 6 ka. Climate Dynamics 12, 185–194), we modified the pollen-PFT and PFT-biomes assignation of Thompson and Anderson (Thompson, R.S., Anderson, K.H., 2000. Biomes of western North America at 18,000; 6000 and 0 14C yr BP reconstructed from pollen and packrat midden data. Journal of Biogeography 27, 555–584) for a better representation of the modern vegetation of NW Mexico. The biome reconstruction method was validated with the modern pollen sites and applied to the fossil sites. Our results show that, during the early Holocene, a cool conifer forest extended at least down to 1700 m, while today this biome is present above 2000 m in the Chihuahua state. The Younger Dryas event was recorded in one site with cold and dry conditions. The reconstructed annual temperature for this period was 3°–6 °C colder than today, and annual precipitation was 250 mm lower than at present (900 mm/yr). The middle Holocene after 9200 cal yr BP was marked by a warming trend, reaching temperatures 2 °C warmer than today at 7000 cal yr BP, and by the installation of a warm mixed forest, the present day biome, at 1700 m elevation, while at higher elevations (1900 m) the cool conifer forest was still present. Summer precipitation was 200 mm/yr above the early Holocene values, suggesting that monsoon-like conditions strengthened since 9200 cal yr BP at this region. During the last 4000 yr, the same warm mixed forest was reconstructed below 1700 m and a conifer forest above 1700 m. A great variability of vegetation and climate patterns was recorded for the last 3000 yr particularly at high elevation sites, where warming and cooling trends would be coeval of the Medieval warm period and Little Ice Age, likely related to ENSO variability.  相似文献   

3.
We report the discovery and classification of 30 new meteorites found in or close to Roosevelt County, New Mexico, including two H3 chondrites and a ureilite; the others are equilibrated ordinary chondrites. Over 160 meteorites representing at least 100 different falls have been recovered from this region, mostly from wind blowout areas. As in Antarctica, small specimens predominate and irons, achondrites and C and E chondrites are rare. Paired specimens are also very difficult to identify.  相似文献   

4.
TIGRE at La Luz Observatory, Guanajuato, Mexico (see J.H.M.M. Schmitt et al., this issue, p. 787). (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

5.
A sample of 100 Sbc galaxies has been observed at different wavelengths and resolutions. The ultimate aim of the project is to probe the origin of their nuclear activity, e.g., blackhole, starbust, etc.The results from radio observations with the VLA (New Mexico) at 20 and 6 cm, with a resolution of 1–2 arc sec, for the inner kpc of nineteen sources are presented. Six of the galaxies show extended emission consistent with starburst activity. The remaining thirteen are unresolved or marginally resolved compact sources. Their steep spectra indicate synchrotron emission. They show total nuclear energies similar to those found for a sample of Seyfert galaxies.Optical spectroscopic observations with a similar resolution to the radio data have been made for approximately 90 galaxies. A sample of the derived rotation curves is included.  相似文献   

6.
Four new irons are described; Buenaventura (IIIB) from Chihuahua, Mexico: mass 114 kg; Denver City (anomalous) from Texas, USA: mass 26.1 kg; Kinsella (IIIB) from Alberta, Canada: mass 3.7 kg; and Tacoma (IA) from Washington, USA: mass 17 g. Denver City is unique, i.e., not related to any other known iron. Tacoma is the smallest iron meteorite recorded. All were purchased for the UCLA collection following a publicity drive for new meteorites  相似文献   

7.
Abstract— A shower of meteorite fragments fell at ～0730 h local time on 1998 June 13 near the town of Portales, New Mexico. Thus far, 51 pieces of the Portales Valley (H6) meteorite have been recovered. This meteorite has an unusually large number of metallic veins. Some of these veins are also unusually thick, having widths on the order of centimeters. These wide veins have fine Widmanstätten structure, which is the first time it has been seen in an ordinary chondrite. This structure indicates the metallic veins and the host chondrite cooled slowly. These veins appear to have been produced by shock-metamorphic processes, which we infer produced a >20 km diameter impact crater on an H-chondrite planetesimal.  相似文献   

8.
By studying the data from the worldwide neutron monitor network the spectra of most of the solar proton events in cycles 19–20 have been determined. These spectra are best represented by a power law with an upper cutoff R m . This holds over a wide range in energy or rigidity. For the events examined R m had values between 3 GV and 20 GV. It is shown that there is no correlation between R m and the amplitude of the events.The equation describing continuous particle acceleration in a confining medium is solved in the non-stationary case. This solution shows the existence of a cutoff in the spectrum, and is compared with the experimental results in connection with the problem of particle acceleration time.Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico City, Mexico.  相似文献   

9.
The Chinese first reported the Crab Nebula supernova on 1054 July 5. Ecclesiastical documents from the near east reported it in April and May of 1054. More than 33 petroglyphs made by Native Americans in the US and Mexico are consistent with sightings both before and after conjunction with the Sun on 1054 May 27. We found a petroglyph showing the new star close to Venus and the Moon, which occurred on 1054 April 12 and April 13, respectively. Collins et al., using the four historical dates, derived a light curve that is like that of a Type Ia supernova. The only remaining problem with this identification is that this supernova was near maximum light for 85 d, which is unlike the behavior of any known supernova.  相似文献   

10.
Late Eocene crystal-bearing spherules have been found in deep sea cores from the Caribbean Sea, Gulf of Mexico, equatorial Pacific Ocean, and eastern equatorial Indian Ocean. Keller et al. (1987) have suggested that the spherules from the western equatorial Pacific (Site 292, core 38) and eastern Indian Ocean (Site 216) are older (Globigerapsis semiinvoluta Zone) than those from the central equatorial Pacific, Gulf of Mexico, and Caribbean Sea (Globorotalia cerroazulensis Zone). The strongest argument in favor of two layers is the biostratigraphic data; however, published biostratigraphic interpretations are at odds with Keller et al.'s (1987) conclusions. Furthermore, paleomagnetic data for Site 292 seems to contradict Keller et al.'s conclusion that the spherules found in core 36 occur in sediments of the same stratigraphic age as those found in the central equatorial Pacific, Gulf of Mexico, and Caribbean Sea sites. Although the spherules from Sites 216 and 292 (core 38) do have higher average CaO, and lower average Al2O3 and FeO contents than the late Eocene spherules from the other sites, there is a great deal of overlap in composition. It is our opinion that the similarities in composition and petrography between the late Eocene crystal-bearing spherules are greater than the differences. Additionally, there seems to be a systematic change in composition and in amount of iridium excess from east to west when all the sites containing the crystal-bearing spherules are considered. We believe, therefore, that it is likely that the late Eocene crystal-bearing spherules all belong to a single event.  相似文献   

11.
Abstract— Five new ordinary chondrites from Roosevelt County, New Mexico, USA, have been assigned to a chemical group, petrologic type and shock stage. All five are moderately to heavily weathered. They are: RC 073, H5(S2); RC 074, L5(S3); RC 076, L4(S3); RC 077 , L4(S2); RC 078, L4(S2).  相似文献   

12.
We have examined the characteristics of the unusual worldwide fluctuations of cosmic-ray intensity on July 14–15, 1961, using corrected hourly data from global network of neutron and meson detectors. A careful study of the associated solar, interplanetary and geophysical phenomena has also been made. These investigations lead us to recognise the dominant role played by the Interplanetary Magnetic Field Inhomogeneities (IMFI) in modulating galactic cosmic-ray flux received at earth during recovery from Forbush decreases. When approaching the earth from the sunward side the IMFI's scatter galactic cosmic rays diffusing towards solar equatorial plane from higher heliolatitudes on to the interplanetary magnetic-field lines which connect to earth. When propagating past the orbit of the earth, the IMFI's set up a flow of scattered galactic cosmic-ray flux in the general direction of the earth. Most of these cosmic rays probably sink in the sun. Transient Spatial Anisotropies are thus set up in the vicinity of the earth in cosmic-ray intensity as viewed by ground-based detectors. Depending upon the relative position of the region abounding in IMFI's and the earth, these short-lived anisotropies appear either from sunward or antisun directions. Sometimes the configuration is such as to set up bidirectional anisotropies. Implications of this broad picture are discussed qualitatively.Our analysis also enables us to place constraint on the mechanism responsible for heating the solar corona over active regions, which we feel must be taken into account by all theoretical models on the subject.This research is supported in part by U.S. Air Force Office of Scientific Research under grant AF-AFOSR-319-66. The paper was presented at the Tenth International Conference on Cosmic Rays, Calgary, June 18–29, 1967.Now at the Dept. of Physics and Astronomy, University of New Mexico, Albuquerque, N.M., U.S.A.  相似文献   

13.
We examine the effects of acoustic-gravity waves with long and short periods on the solar profile of the K i7699 line using a dynamic model of line formation.First we studied the kinetic equilibrium of the K i atoms in a static atmosphere confirming, with up-to-date atomic data and atmospheric model, that a good fit of the resonance line 7699 is possible only when non-LTE effects are accounted for.Then the static non-LTE line source function and lower-level population are used as input data for calculating the line formation in the presence of waves.The time behaviour of the synthetic profiles corresponding to 300 s and 30 s waves is extensively discussed. The characteristic redshift induced by the 30 s wave is explained within the framework of the S-S line formation model. Long-period waves yield an anticorrelation between the asymmetry at different residual intensities and the line core shift, as observed. The short-period waves with velocity amplitude of about 100 m s–1 (at the base of the photosphere) produce a mean bisector whose lower part has a slope in agreement with the observed one. The efficiency of waves to produce macro and microturbulence is also discussed.Currently NAS/NRC Senior Research Associate at Sacramento Peak Obs., New Mexico, U.S.A.  相似文献   

14.
Analyses of Martian surface soil by Viking and Earth-based telescopes have been interpreted as indicating a regolith dominated by the weathering products of mafic or ultramafic rocks. Basaltic glass has previously been proposed as a more likely precursor than crystalline rock, given the low efficiency of surface weathering under present Martian conditions. On Earth large volumes of basaltic glass formed by quenching of magma by water. A similar interaction, between magma and ground ice, may have been a common occurrence on Mars. On the basis of this scenario palagonite, the alteration product of basaltic sideromelane glass, was studied as a possible analog to Martian soil. Samples from Iceland, Alaska, Antarctica, Hawaii, and the desert of New Mexico and Mexico were examined by optical and scanning electron microscopy, electron microprobe analysis, X-ray diffraction, spectrophotometry, and magnetic and thermogravimetric analysis. We suggest that palagonite is a good analog to the surface soil of Mars in chemical composition, particle size, spectral signature, and magnetic properties. Our model for the formation of fine-grained Martian surface soil begins with eruptions of basaltic magma through ground ice, forming deposits of glassy tuff. Individual glass shards are then altered by low-temperature hydrothermal systems to palagonitic material. Dehydration and aeolian abrasion strip the alteration rinds from the glass, and wind storms distribute the silt-sized palagonitic fragments in a planet-wide deposit.  相似文献   

15.
本文概述１９９１年７月１１日日全食时中国日食观测队在墨西哥ＬａＰａｚ所作的近红外光谱观测情况及得到的初步结果。观测是用一强光力望远镜和一中小色散的光谱仪，配以ＣＣＤ摄象机、图象处理器、微机等组成的探测系统进行的。日全食时，在λ１０７１２－１０９７２波区共摄得极上层光球和色球的无缝光谱４１帧。日面外约１．０９６Ｒ处的有缝光谱３５帧。文中还介绍了拍得的色球、日珥资料概况。  相似文献   

16.
The Multi-Spectral Solar Telescope Array (MSSTA), a rocket-borne solar observatory, was successfully launched from White Sands Missile Range, New Mexico, on May 13, 1991 at 19:05 UT. The telescope systems onboard the MSSTA obtained several full disk solar images in narrow bandpasses centered around strong soft X-ray, EUV, and FUV emission lines. Each telescope was designed to be sensitive to the coronal plasmas at a particular temperature, for seven temperatures ranging from 20000 K to 4000000 K. We report here on the images obtained during the initial flight of the MSSTA, and on the chromospheric and coronal structure of polar plumes observed over both poles of the Sun. We have also co-aligned the MSSTA images with Kitt Peak magnetograms taken on the same day. We are able to positively identify the magnetic structures underlying the polar plumes we analyze as unipolar. We discuss the plume observations and present a radiative energy balance model derived from them.  相似文献   

17.
Abstract— Four exposures of Chicxulub impact ejecta along the Mexico‐Belize border have been sampled and analyzed for major and trace element abundances. The ejecta deposits consist of a lower spheroid bed, containing clay and dolomite spheroids, and an upper diamictite bed with boulders and clasts of limestone and dolomite. The matrix of both beds is composed of clay and micritic dolomite. The rare earth element (REE) compositions in the matrix of both units show strong similarities in concentrations and pattern. Furthermore, the Zr/TiO2 scatter plot shows a linear correlation indicating one source. These results indicate that the basal spheroid bed has the same source and was generated during the same event as the overlying diamictite bed, which lends support to a single‐impact scenario for the Albion Formation ejecta deposits. The elevated concentrations of non‐meteoritic elements such as Sb, As, U, and Zn in the matrix of the lower spheroid bed are regarded to have been derived from the sedimentary target rocks at the Chicxulub impact site. The positive Eu and Ce anomalies in clay concretion and in the matrix of the lower part of the spheroid bed in Albion Island quarry is probably related to processes involved in the impact, such as high temperature and oxidizing conditions. Analogous trace element anomalies have been reported from the distal Cretaceous‐Paleogene (K/T) boundary clay layer at different sites. Thus, the trace element signals, reported herein, are regarded to support a genetic link between the Chicxulub impact, the ejecta deposits along the Mexico‐Belize border, and the global K/T boundary layer.  相似文献   

18.
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19.
We present first results of the photometric and spectroscopic investigation of the B1/B2 Herbig star HD52721 performed in 2009–2010 at three observatories: Mountain Astronomical Station (Kislovodsk)—photometry, CrAO (Crimea, Ukraine)—spectroscopy, Observatory San Pedro Martyr (Ensenada, Mexico)—high-resolution echelle-spectroscopy. We have also used photometric data from the ASAS survey for 2003–2009. Our analysis has shown that a) the object is a close binary system with the orbital period of 1.610 days composed of two components of similar spectral type (B1–B2); b) the system is surrounded by the common disk-like envelope containing azimuthal inhomogeneity rotating with the orbital period of the system. We present preliminary estimates of the system parameters and discuss its possible nature.  相似文献   

20.
Novae and arachnoids are Venusian structures, both supposedly formed by a volcanic uplifting (Janes et al., Lunar Planet. Sci. XXVII (1996) 605; Head et al., J. Geophys. Res. 97 (E8) (1992) 13,153). Corona-like features and radially fractured domes, which could be considered as novae, have been connected to the coronae or the corona formation (Squyres et al., J. Geophys. Res. 97 (E8) (1992) 13,153; Stofan et al., J. Geophys. Res. 97 (E8) (1992) 13,347). Arachnoids are also thought to be a sub-type of coronae (Price and Suppe, Earth Moon Planets 71 (1995) 99) or corona-like features (Head et al., 1992). Despite the fact that they both belong to the same broad class of corona and corona-like features, these structures seem to have very divergent basic characteristics generally. In addition to morphological differences, the novae are mostly elevated in a distinct way with lava flows and radial fractures while the majority of the arachnoids are structures with depressed interior, radial ridges and they are without lava flows. The distribution map indicates that the novae are located in sparse chains on the deformation belts and the arachnoids are in groups or in clusters on the plains. On the area to the south of Atla Regio, novae and arachnoids seem to be rather densely spaced, but also within this region the novae are on the extension zones and most of the arachnoids are located on the plains or adjoining a ridge belt. Only the few arachnoids which are located in some uncommon location, such as close to an extension zone or within a volcanic area, display some properties that usually are found in novae. This indicates that the geologic environment is a significant factor in the formation process of novae and arachnoids.  相似文献   

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