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1.
We have carried out an analysis of the (0, 0) vibrational band of the CN molecule in Comet Mrkos 1957d, including the effect of collisions. We found that the sum of the squares of the residuals can be reduced by a factor of ten, if collisions account for 46±3% of the population of the lower level. A rotational temperature can be assigned to the cometary gas. The best value found was 410±40 K. The best fit for the constantR 1 was (1.07±0.10)×10–4. The velocity of the comet was left as a free parameter. We found for it a value of 34.38±0.10 km s–1. This result is in disagreement with the nuclear orbital velocity of 34.74 km s–1. The discrepancy can be explained, if the CN molecules are ejected from the cometary nucleus preferentially in the sunward direction, with a mean velocity that corresponds to the above temperature.  相似文献   

2.
Limb-darkening tables for blanketed model atmospheres fitted to main sequence stars in the F0-K0 spectral range are presented. The tables cover the wavelength range 3646-24000.  相似文献   

3.
Uncertainties in the fundamental line profiles and absorption strengths in HD are among the most important sources of error in the analysis of the spectra of HD in the atmosphere of the outer planets. Measurements of the 4-0, 5-0, and 6-0 vibrational bands of HD, taken at room temperature and a range of densities from 0.3 to 1.7 amagat are reported. High S/N spectra have been obtained at a spectral resolution finer than the natural line widths, allowing analysis of spectral profiles, absorption strengths, and pressure shifts in the HD lines. Line profiles are interpreted in terms of the theoretical Galatry approximation, and the HD pressure-broadening and self-diffusion coefficients are determined as free parameters.  相似文献   

4.
The inhomogeneous Bianchi type-VI0 perfect fluid solution given recently by Roy and Narain (1985) is shown to be identical with the solution first given by Tomita (1978).  相似文献   

5.
Altimetric measurements of the GEOSAT satellite were used for the determination of geopotential scale factorR 0. The geopotential valueW 0 on the geoid surface was then computed (W 0 =GM/R 0).The GEOSAT Geophysical Data Records (GDR's) covering an initial period of the Exact Repeat Mission (ERM) were filtered and processed. The necessary corrections were made in order to allow a precise detection of the sea surface. Gravitational geopotential, rotation and permanent tides were taken into account and the equipotential surface which is the best approximation of the sea surface was found.The determination of the potential valueW 0 on the mean geoid surface in this way is very promising. An associated value withW 0 - the geopotential scale factorR 0 - seems to be a very good Earth dimension defining quantity. Moreover, there are many possible applications ofW 0 (R 0) in modern geophysics.The incorporation of one of these parameters - we now recommendR 0 - into the set of the Primary Geodetic Parameters (PGP) is discussed and suggested.  相似文献   

6.
We investigate a one-zone chemo-photometric evolutionary model of truncated spiral galaxies with and without starbursts in order to explore the origin of the spectrophotometric properties of S0s. First, we show that 1) the tight U-V colour–magnitude (CM) relation cannot reject the model with a starburst and 2) the model with a starburst can explain the difference in the I-K colour–magnitude relation between S0 galaxies and spiral galaxies. Next, we demonstrate how we can distinguish the truncated spirals with a starburst from those without a starburst by using the CaII–Hδ/λ4045 diagram (proposed by Leonardi and Rose, 1996) and the 1550-V colour. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

7.
The exterior field of the Bianchi type-VI0 metric in the Lyttleton-Bondi universe is considered and an exact cosmological model is presented. Some physical properties of the model are discussed.  相似文献   

8.
We present Gemini Multi-Object Spectrograph longslit spectroscopy of the isolated S0 galaxy NGC 3115. We have determined kinematical data and Lick/IDS absorption line-strength indices for the major axis out to around 9 kpc and for the minor axis out to around 5 kpc (around 2R e ). Using stellar population models which include the effects of variable [α/Fe] ratios, we derive metallicities, abundance ratios and ages for the stellar population of NGC 3115. We find that [α/Fe] remains fairly constant with increasing radius at around  [α/Fe]= 0.17  for the major axis but increases rapidly for the minor axis to around  [α/Fe]= 0.3  . We also find that to first order, this behaviour can be explained by a simple spheroid + disc model, where the spheroid has  [α/Fe]= 0.3  and the disc shows close to solar abundance ratios. The disc also appears considerably younger than the spheroid, having an age of around 6 Gyr compared to 12 Gyr for the spheroid. We compare these results to those previously presented for the globular cluster system of NGC 3115.  相似文献   

9.
We wish to point out that the Brans-Dicke-Bianchi type-VI0 stiff matter solution recently given by Ram and Singh is not the most general solution of the corresponding field equations. Moreover, this solution has no vacuum limit and the general relativistic limit is obtained only after making an asymptotic expansion. In this paper we rediscuss the entire problem in a different way. In the limit =const., , we obtain both the stiff matter and the vacuum relativistic limit first given by Ellis and MacCallum (1969) in analytic form.  相似文献   

10.
Co-ordinated rocket measurements of the O2(a1Δg−X3Σg−) Infrared Atmospheric (0-0) band emission profile and the atomic oxygen densities in an undisturbed night-time atmosphere are used to investigate the processes responsible for the excitation of O2(a1Δg) in the terrestrial nightglow. It is shown that three-body recombination of atomic oxygen, and subsequent energy transfer processes, can explain only part of the observed emission profile and that at least two other sources of O2(a1Δg) emission must exist. One of these additional sources, responsible for most of the emission observed below 90km, is identified as arising from the night-time residual of the very large dayglow 1Δg population. The other additional source is required to explain most of the emission observed above 95km. The processes responsible for this high altitude component cannot be identified but the vertical distribution of the required source function strongly resembles the profile of the atomic oxygen density squared and suggests that a two-body radiative recombination process may be involved. However, the measured zenith emission rates can also be explained without the high altitude source of O2(a1Δg) if optical emission at 1.27 μm was induced by the rocket as it penetrated the nightglow layer.  相似文献   

11.
Climatic changes over the Mediterranean basin in 2031–2060, when a 2 °C global warming is most likely to occur, are investigated with the HadCM3 global circulation model and their impacts on human activities and natural ecosystem are assessed. Precipitation and surface temperature changes are examined through mean and extreme values analysis, under the A2 and B2 emission scenarios. Confidence in results is obtained via bootstrapping. Over the land areas, the warming is larger than the global average. The rate of warming is found to be around 2 °C in spring and winter, while it reaches 4 °C in summer. An additional month of summer days is expected, along with 2–4 weeks of tropical nights. Increase in heatwave days and decrease in frost nights are expected to be a month inland. In the northern part of the basin the widespread drop in summer rainfall is partially compensated by a winter precipitation increase. One to 3 weeks of additional dry days lead to a dry season lengthened by a week and shifted toward spring in the south of France and inland Algeria, and autumn elsewhere. In central Mediterranean droughts are extended by a month, starting a week earlier and ending 3 weeks later. The impacts of these climatic changes on human activities such as agriculture, energy, tourism and natural ecosystems (forest fires) are also assessed. Regarding agriculture, crops whose growing cycle occurs mostly in autumn and winter show no changes or even an increase in yield. In contrast, summer crops show a remarkable decrease of yield. This different pattern is attributed to a lengthier drought period during summer and to an increased rainfall in winter and autumn. Regarding forest fire risk, an additional month of risk is expected over a great part of the basin. Energy demand levels are expected to fall significantly during a warmer winter period inland, whereas they seem to substantially increase nearly everywhere during summer. Extremely high summer temperatures in the Mediterranean, coupled with improved climate conditions in northern Europe, may lead to a gradual decrease in summer tourism in the Mediterranean, but an increase in spring and autumn.  相似文献   

12.
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13.
Astronomy Letters - We present the results of our spectroscopic study of the lenticular galaxy NGC 4143—a peripheral member of the Ursa Major cluster. Using the observations at the 6-m SAO...  相似文献   

14.
Acounter-rotating gas disk has been detected in the SA0 galaxy IC 560 located at the periphery of a sparse group of six late-type galaxies. The pattern of gas excitation and mid-infrared colors are indicative of ongoing star formation within 1 kpc of the center. Outside the gas disk with star formation the large-scale stellar disk of the galaxy has an old age and a very low metallicity, [Z/H] ≈ ?1. The source of external gas accretion onto IC 560 is undetected; the only option is a single infall of a companion rich in high-metallicity gas.  相似文献   

15.
When and how red S0 galaxies were formed is a longstanding and noteworthy problem. Recent morphological and photometric studies of S0sin distant clusters of galaxies have revealed a smaller S0 population fraction and the existence of S0s with bluer colours, which suggests that some physical processes drive continuous creation of S0s with younger stellar populations in higher-redshift clusters. We propose here that the major mechanism for S0 creation is galaxy merging between two spirals of unequal masses. Our numerical simulations demonstrate that galaxy merging exhausts a large amount of the interstellar medium of two gas-rich spirals owing to the moderately enhanced star formation, and subsequently transforms the two into a single gas-poor S0 galaxy with structure and kinematics strikingly similar to those observed. This secondary S0 formation via unequal-mass merging thus provides an evolutionary link between a larger number of blue spirals observed in intermediate-redshift clusters and the red S0s prevalent in present-day ones. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

16.
We produce and analyse u -band (  λ≈ 355  nm) luminosity functions (LFs) for the red and blue populations of galaxies using data from the Sloan Digital Sky Survey (SDSS) u -band Galaxy Survey ( u GS) and Deep Evolutionary Exploratory Probe 2 (DEEP2) survey. From a spectroscopic sample of 41 575 SDSS u GS galaxies and 24 561 DEEP2 galaxies, we produce colour magnitude diagrams and make use of the colour bimodality of galaxies to separate red and blue populations. LFs for eight redshift slices in the range  0.01 < z < 1.2  are determined using the  1/ V max  method and fitted with Schechter functions showing that there is significant evolution in   M *  , with a brightening of 1.4 mag for the combined population. The integration of the Schechter functions yields the evolution in the u -band luminosity density (LD) out to   z ∼ 1  . By parametrizing the evolution as  ρ∝ (1 + z )β  , we find that  β= 1.36 ± 0.2  for the combined populations and  β= 2.09 ± 0.2  for the blue population. By removing the contribution of the old stellar population to the u -band LD and correcting for dust attenuation, we estimate the evolution in the star formation rate (SFR) of the Universe to be  βSFR= 2.5 ± 0.3  . Discrepancies between our result and higher evolution rates measured using the infrared and far-UV can be reconciled by considering possibilities such as an underestimated dust correction at high redshifts or evolution in the stellar initial mass function.  相似文献   

17.
We present Galaxy Ultraviolet Explorer (GALEX) satellite observations of the SB0 galaxy NGC 4262 where we detect an extended, outer ring studded with UV-bright knots surrounding the galaxy body. Such a structure, not visible at optical wavelengths, is coupled with a ring of atomic (HI) gas. We will show that both star-forming and HI rings surrounding this SB0 galaxy share the same radial distance from the galaxy center and spatial orientation. We also model the kinematics of the ring(s) and of the galaxy body. Their kinematics is not coupled with that of the galaxy stars. We suggest that NGC 4262 has undergone a major gas stripping event in the past that was the origin of the present “necklace” of UV-bright knots.  相似文献   

18.
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19.
An exact Bianchi type-VI0 cosmological model in the presence of zero-mass scalar fields is obtained when the source of the gravitational field is a perfect fluid with pressure equal to energy density. Some physical properties of the model are discussed.  相似文献   

20.
In the Kepler/K2 data analysis performed to date, aperture photometry has generally been used, but this method has not given any reasonable results when examining nearby sources due to the insufficient number of pixels on Kepler's CCD camera. The point-spread function (PSF) technique prepared by Libralato et al. (2016a), which presents promising results in undersampled pixels even in crowded star groups, was used in this study. Open cluster stars M 35 and NGC 2158 in the K2 Campaign 0 were selected as the target field. By applying the PSF method to the high angular resolution input catalogue prepared using the Asiago Schmidt telescope, M 35 and NGC 2158 provided the opportunity to examine the light curves of faint stars (Kp > 15.5) in crowded regions and gave better results compared to aperture photometry. In this study, I detrended ~50 000 raw light curves from systematic effects and spacecraft motion effects. I ultimately found two candidate host stars that could have possible planetary transits.  相似文献   

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