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1.
《Planetary and Space Science》1999,47(3-4):327-330
The asteroid 85 Io has been observed using CCD and photoelectric photometry on 18 nights during its 1995–96 and 1997 apparitions. We present the observed lightcurves, determined colour indices and modelling of the asteroid spin vector and shape. The colour indices (U-B = 0.35±0.02, B-V = 0.66±0.02, V-R = 0.34±0.02, R-I = 0.36±0.02) are as expected for a C-type asteroid. The allowed spin vector solutions have the pole co-ordinates λ0 = 285±4°, β0 = −52±9° or λ0 = 108±10°, β0 = −46±10° and λ0 = 290±10°, β0 = −16±10° with a retrograde sense of rotation and a sidereal period Psid = 0d.286463±0d.000001. During the 1995–96 apparition the International Occultation Time Association (IOTA) observed an occultation event by 85 Io. The observations and modelling presented here were analysed together with the occultation data to develop improved constraints on the size of the asteroid. The derived value of 164 km is about 5% larger than the IRAS diameter. © 1999 Elsevier Science Ltd. All rights reserved.  相似文献   

2.
The results of photometric astrometry, a method of determining the orientation of a rotation axis, as applied to asteroid 44 Nysa are presented. The pole orientation of Nysa was found to be λ0 = 100°, β0 = +60° with an uncertainty of 10°. The sidereal period is 0d.26755902 ± 0.00000006, and the rotation prograde. Refinements to, and limitations of, the application of the method of photometric astrometry are discussed. In light of the results presented herein, we believe that all photometric astrometry pole determinations of the past should be redone.  相似文献   

3.
Further reduction of Doppler tracking data from Mariner 9 confirms our earlier conclusion that the gravity field of Mars is considerably rougher than the fields of either the Earth or the Moon. The largest positive gravity anomaly uncovered is in the Tharsis region which is also topographically high and geologically unusual. The best determined coefficients of the harmonic expansion of the gravitational potential are: J2 = (1.96 ± 10.01) × 10?3 ; C22 = ?(5.1 ± 0.2) × 10?5; and S22 = (3.4 ± 0.2) × 10?5. The other coefficients have not been well determined on an individual basis, but the ensemble yields a useful model for the gravity field for all longitudes in the vicinity of 23° South latitude which corresponds to the periapse position for the orbiter.The value obtained for the inverse mass of Mars (3 098 720 ± 70 M⊙?1) is in good agreement with prior determinations from Mariner flyby trajectories. The direction found for the rotational pole of Mars, referred to the mean equinox and equator of 1950.0, is characterized by α = 317°.3 ± 0°.2, δ = 52°.7 ± 0°.2. This result is in excellent agreement with Sinclair's recent value, determined from earth-based observations of Mars' satellites, but differs by about 0°.5 from the previously accepted value. Other important physical constants that have either been refined or confirmed by the Mariner 9 data include: (i) the dynamical flattening, f = (5.24 ± 0.02) × 10?3; (ii) the maximum principal moment of inertia, C = (0.375 ± 0.006) MR2; and (iii) the period of precession of Mars' pole, P ? (1.73 ± 0.03) × 105 yr, corresponding to a rate of 7.4 sec of arc per yr.  相似文献   

4.
Nineteen new lightcurves of 16 Psyche are presented along with a pole orientation derived using two independent methods, namely, photometric astrometry (PA) and magnitude-amplitude-shape-aspect (MASA). The pole orientations found using these two methods agree to within 4°. The results from applying photometric astrometry were prograde rotation, a sidereal period of 0ddot1748143 ± 0ddot0000003, and a pole at longitude 223° and latitude +37°, with an uncertainty of 10°; and, from applying magnitude-amplitude-shape-aspect a pole at 220 ± 1°, +40 ± 4°, and a modeled triaxial ellipsoid shape (a > b > c) with a/b = 1.33 ± 0.02 and b/c = 1.33 ± 0.07. The discrepancy between the high pole latitude found here and the low latitudes reported by others is discussed.  相似文献   

5.
We have redetermined the kinematic parameters of the Gould Belt using currently available data on the motion of nearby young (log t < 7.91) open clusters, OB associations, and moving stellar groups. Our modeling shows that the residual velocities reach their maximum values of ?4 km s?1 for rotation (in the direction of Galactic rotation) and +4 km s?1 for expansion at a distance from the kinematic center of ≈300 pc. We have taken the following parameters of the Gould Belt center: R 0 = 150 pc and l 0 = 128°. The whole structure is shown to move relative to the local standard of rest at a velocity of 10.7 ± 0.7 km s?1 in the direction l = 274° ± 4° and b = ?1° ± 3°. Using the derived rotation velocity, we have estimated the virial mass of the Gould Belt to be 1.5 × 106 M ⊙.  相似文献   

6.
To study the peculiarities of the Galactic spiral density wave, we have analyzed the space velocities of Galactic Cepheids with propermotions from the Hipparcos catalog and line-of-sight velocities from various sources. First, based on the entire sample of 185 stars and taking R 0 = 8 kpc, we have found the components of the peculiar solar velocity (u ⊙, v ⊙) = (7.6, 11.6) ± (0.8, 1.1) km s?1, the angular velocity of Galactic rotation Ω0 = 27.5 ± 0.5 km s?1 kpc?1 and its derivatives Ω′0 = ?4.12 ± 0.10 km s?1 kpc?2 and Ω″0 = 0.85 ± 0.07 km s?1 kpc?3, the amplitudes of the velocity perturbations in the spiral density wave f R = ?6.8 ± 0.7 and f θ = 3.3 ± 0.5 km s?1, the pitch angle of a two-armed spiral pattern (m = 2) i = ?4.6° ± 0.1° (which corresponds to a wavelength λ = 2.0 ± 0.1 kpc), and the phase of the Sun in the spiral density wave χ⊙ = ?193° ± 5°. The phase χ⊙ has been found to change noticeably with the mean age of the sample. Having analyzed these phase shifts, we have determined the mean value of the angular velocity difference Ω p ? Ω, which depends significantly on the calibrations used to estimate the individual ages of Cepheids. When estimating the ages of Cepheids based on Efremov’s calibration, we have found |Ω p ? Ω0| = 10 ± 1stat ± 3syst km s?1 kpc?1. The ratio of the radial component of the gravitational force produced by the spiral arms to the total gravitational force of the Galaxy has been estimated to be f r0 = 0.04 ± 0.01.  相似文献   

7.
Hans Josef Schober 《Icarus》1976,28(3):415-420
The minor planet 79 Eurynome was observed during the 1974 opposition for four nights in November, using a photoelectric photometer attached to the 60 cm telescope at the Observatoire de Haute Provence, France. A synodic period of Psyn = 5h 58m46s ± 6s m.e. was derived. The total amplitude of the lightcurve is only 0.05 mag. The lightcurve shows a double maximum and double minimum. Both minima appear to be at the same level. Observations were carried out in an instrumental filter system (UBV)' Results are shown only for V′, but U′ and B′ measurements supplement the conclusions concerning the rotation. The phase angle α, covered by the observations, ranges from 3 to 5°. The present results for 79 Eurynome rule out the longer period of 0d.49830 derived by F. Scaltriti and V. Zappalà in favor of their possible period of 0d.24915.  相似文献   

8.
By means of new photoelectric observations made in 1974 an attempt to determine the poles of asteroids 9 and 44 was made. Following a method based upon the magnitude-aspect and amplitude-aspect relations, the coordinates of the poles for 9 and 44 were found to be, respectively, λ0 = 191° ± 5°, β0 = 56° ± 6° and λ0 = 100° ± 10°, β0 = 50° ± 10°. The previously published pole for asteroid 22, λ0 = 215° ± 10°, β0 = 45° ± 15°, was confirmed. From its phase relation we determined the phase coefficient of 44 Nysa, a very high albedo object (pv = 0.377). The very low phase coefficient obtained (βv = 0.018 mag/deg) agrees very well with an inverse relation between geometrical albedo and phase coefficient. The results are summarized in a table.  相似文献   

9.
One sensor of the Helios micrometeoroid experiment is covered by a thin film consisting of 3000 Å parylene and 750 Å aluminium. Micrometeoroids must penetrate this film before they are detected. In order to study the effects of the film on the detection of micrometeoroids simulation experiments were performed with iron, aluminium, glass and polyphenylene projectiles in the mass range of 5 × 10?13g < m < 2 × 10?10g and in the speed range of 1.5 km/sec <ν < 13 km/sec. The bulk densities of the projectiles ranged from 1.25 g/cm3 (polyphenylene) to 7.9 g/cm3 (iron). By measuring the speed of the projectiles before and after the film penetration the speed loss Δν caused by the film was determined. The angle of incidence was varied in three steps (0°, 30° and 60°). This deceleration strongly depends on the projectiles' densities: Vertically impacting iron projectiles of m = 10?11g and ν1 = 3 km/sec were subject to a relative speed loss of Δν/ν1 = 4%, aluminium projectiles of the same mass and speed showed Δν/ν1 = 8%, glass projectiles Δν/ν1 = 9% and polyphenylene projectiles Δν/ν1 = 14%. The total charge of the plasma produced upon impact on a gold target of a projectile which had penetrated the film before that was compared with the plasma produced by a projectile without a penetration. For iron projectiles these two signals did not differ significantly even at an angle of incidence of 60°. Whereas polyphenylene projectiles showed an attenuation of the charge signal by a factor of 10 after the penetration already at an angle of incidence of 0°. Polyphenylene projectiles impacting the film at an angle of incidence of 60° could no longer be detected behind the film. This experiment defined the penetration limit of the Helios film. Comparison with other penetration data yielded a penetration formula which is applicable to projectiles with diameters in the submicron to centimeter range. This penetration formula gives the penetration limit of a film as a function of the projectile's mass, speed and density.  相似文献   

10.
We used observations at 4 oppositions to calculate the rotation of the asteroid (16) Psyche. Our results are 1) the pole is λ 225°, β = +5° (1950.0), 2) the rotation is direct, and 3) the sidereal period is 4h 11m 45s.42 ± 0s.01.At the three oppositions of 1955, 1965 and 1980, the relative positions of the Sun, the Earth and the asteroids were almost the same, and the observed light curves were also nearly the same. Therefore, this asteroid may be said to have shown no precession over the 20 years observed.  相似文献   

11.
The period of the β Cephei variable, BW Vulpeculae, is increasing all the time at a rate of (14.24±0.20) × 10?10d/d. Also, the residual in the time of light maximum shows a quasi-sinusoidal variation with a period of about 26.3 years and an amplitude of 0.022 – 0.024 days. If this is interpreted as the light-time effect in a binary orbit, then the orbit will have a size a sin i = 1.91 – 2.08 AU and an eccentricity e = 0.52.  相似文献   

12.
J.L. Dunlap 《Icarus》1976,28(1):69-78
Ten lightcurves and UBV photometry of 433 Eros were obtained between August 1972 and May 1975. The absolute magnitude of the lightcurve maximum is 10.75 and the phase coefficient is 0.025 mag/deg. There may be a small difference in B-V color between the northern and southern hemispheres. The pole of the axis of rotation is directed toward λ0 = 16°, β0 = 12°, ecliptic longitude and latitude, respectively, and the rotation is direct with a sidereal period of 0.d219599 or 5h16m13s4 ± 0.s2. The dimensions derived from the polarimetric albedo and the lightcurve amplitudes are 12km × 12km × 31km for a smooth cylinder with hemispherical ends.  相似文献   

13.
We present the results of photometric observations of a bright cataclysmic variable TT Ari with an orbital period of 0.13755 days. CCD observations were carried out with the Russian-Turkish RTT 150 telescope in 2001 and 2004 (13 nights). Multi-color photoelectric observations of the system were obtained with the Zeiss 600 telescope of SAO RAS in 1994–1995 (6 nights). In 1994–1995, the photometric period of the system was smaller than the orbital one (0 . d 132 and 0 . d 134), whereas it exceeded the latter (0 . d 150 and 0 . d 148) in 2001, 2004. An additional period exceeding the orbital one (0 . d 144) is detected in 1995 modulations. We interpret it as indicating the elliptic disc precession in the direction of the orbital motion. In 1994, the variability in colors shows periods close to the orbital one (0 . d 136, b-v), as well as to the period indicating the elliptic disk precession (0 . d 146, w-b). We confirm that during the epochs characterized by photometric periods shorter than the orbital one, the quasi-periodic variability of TT Ari at time scales about 20 min is stronger than during epochs with long photometric periods. In general, the variability of the system can be described as a “red” noise with increased amplitudes of modulations at characteristic time scales of 10–40 min.  相似文献   

14.
We analyze the peculiar velocity field for 2400 flat spiral galaxies selected from an infrared sky survey (2MFGC). The distances to the galaxies have been determined from the Tully-Fisher relation in the photometric J band with a dispersion of 0m.45. The bulk motion of this sample relative to the cosmic microwave background (3K) frame has an amplitude of 199 ± 37 km s?1 in the direction l = 290° ± 11°, b = +1° ± 9°. The amplitude of the dipole motion tends to decrease with distance in accordance with the expected convergence of bulk flows in the 3K frame. We believe that external massive attractors similar to the Shapley cluster concentration are responsible for ～60% of the local flow velocity in the z = 0.03 volume.  相似文献   

15.
New and existing photometry for the G0 Ia supergiant HD 18391 is analyzed in order to confirm the nature of the variability previously detected in the star, which lies off the hot edge of the Cepheid instability strip. Small‐amplitude variability at a level of δV = 0.016 ± 0.002 is indicated, with a period of P = 123d.04 ± 0d.06. A weaker second signal may be present at P = 177d.84 ± 0d.18 with δV = 0.007 ± 0.002, likely corresponding to fundamental mode pulsation if the primary signal represents overtone pulsation (123.04/177.84 = 0.69). The star, with a spectroscopic reddening of EB–V = 1.02 ± 0.003, is associated with heavily‐reddened B‐type stars in its immediate vicinity that appear to be outlying members of an anonymous young cluster centered ∼10′ to the west and 1661 ± 73 pc distant. The cluster has nuclear and coronal radii of rn = 3.5′ and Rc = 14′, respectively, while the parameters for HD 18391 derived from membership in the cluster with its outlying B stars are consistent with those implied by its Cepheid‐like pulsation, provided that it follows the semi‐period‐luminosity relation expected of such objects. Its inferred luminosity as a cluster member is MV = –7.76 ± 0.10, its age (9 ± 1) × 106 years, and its evolutionary mass ∼19 M⊙. HD 18391 is not a classical Cepheid, yet it follows the Cepheid period‐luminosity relation closely, much like another Cepheid impostor, V810 Cen (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

16.
A.W. Harris  J.W. Young  E. Bowell 《Icarus》1980,43(2):181-183
Photoelectric lightcurves of 304 Olga were obtained at Table Mountain Observatory in 1978 near opposition. From these observations, and several observations made from Lowell Observatory a month later, we obtain a rotation period of 18.36 ± 0.02 hr and lightcurve amplitude of 0m·20. The range of solar phase angle covered by the observations is from 2°·0 to 22°. The resulting phase function is well fit by the Bowell and Lumme model (1979, in Asteroids, T. Gehrels, Ed., pp. 132–169, Univ. of Arizona Press, Tucson), with Q = 0.02. This low value of Q is suggestive of a low-albedo object.  相似文献   

17.
Based on kinematic data on masers with known trigonometric parallaxes and measurements of the velocities of HI clouds at tangential points in the inner Galaxy, we have refined the parameters of the Allen-Santillan model Galactic potential and constructed the Galactic rotation curve in a wide range of Galactocentric distances, from 0 to 20 kpc. The circular rotation velocity of the Sun for the adopted Galactocentric distance R 0 = 8 kpc is V 0 = 239 ± 16 km s?1. We have obtained the series of residual tangential, ΔV θ , and radial, V R , velocities for 73 masers. Based on these series, we have determined the parameters of the Galactic spiral density wave satisfying the linear Lin-Shu model using the method of periodogram analysis that we proposed previously. The tangential and radial perturbation amplitudes are f θ = 7.0±1.2 km s?1 and f R = 7.8±0.7 km s?1, respectively, the perturbation wave length is λ = 2.3±0.4 kpc, and the pitch angle of the spiral pattern in a two-armed model is i = ?5.2° ±0.7°. The phase of the Sun ζ ⊙ in the spiral density wave is ?50° ± 15° and ?160° ± 15° from the residual tangential and radial velocities, respectively.  相似文献   

18.
A concise explanation of studies on distortion of space-time dimension is briefly introduced. Second we obtain the limits (i.e., bounded values) of the dimensionless chemical potential μ, the Sunyaev–Zeldovich (SZ) effect y and distortion of the space-dimension ε by Monte Carlo (MC) analysis of the parameter set (T, d=3+ε, μ, and y) in cosmic microwave data assuming that the SZ effect is positive (y>0). In this analysis, the magnitude of the space-dimension d with distortion of the space-dimension ε is defined by d=3+ε. The limits of μ and y are determined as |μ|<9×10?5 (2σ) (μ=(?3.9±2.6)×10?5 (σ)), |y|<5×10?6 (2σ) (y=(2.0±1.4)×10?6 (σ)), while the distortion of the space-dimension is |ε|<6×10?5 (2σ) (ε=(?0.78±2.50)×10?5 (σ)). The magnitudes of these three estimated limits are ordered as . The estimated limit of |y|<5×10?6 appears to be related to re-ionization processes occurring at redshift z ri ～10. We also present data analysis assuming a relativistic SZ effect.  相似文献   

19.
Auf der Basis von sich über einen Zeitraum von 10 Jahren erstreckenden aerologischen Messungen für den Raum Pozna$ (φ = 52° 24′, $LD = 1h 07m.5, h0 = 85 m) wurde eine statistische Analyse sowohl zeitlicher als auch lokaler Effekte der astronomischen Refraktion durchgeführt. Es wurden keine wahrnehmbaren Effekte zeitlicher Variationen in den höheren Atmosphärenschichten verzeichnet. Damit kann die momentane lokale Refraktion recht exakt durch die mittlere lokale Refraktion approximiert werden, die sich aus einem momentanen Brechungsindex n0 auf dem Grundniveau bestimmt. Es gibt jedoch eine systematische Differenz zwischen der Standardrefraktion, berechnet mittels n0, und der lokalen Refraktion. Dieser Unterschied erweist sich als recht deutlich, so da$sZ es sinnvoll ist, eine lokale Korrektur für die Standardrefraktion einzuführen. Für Poznan ist diese Korrekturgrö$sZe negativ und beläuft sich auf 0″.01 fürz0 = 60°, 0″.1 für z0 = 77°, 1″ für z0 = 85°, und 3″ für z0 = 87°. At z0 = 82°. Für Werte grö$sZer als z0 = 82° überschätzt die Korrektur die Varianz der stochastischen Refraktionsanomalien (Bildbewegung), die über einen Zeitraum von 60 s integriert wurde. Diese Arbeit gibt eine Antwort auf die schon lange diskutierte Frage, ob wir eine lokale reine Refraktion anwenden sollten und wenn ja, in welcher Weise.  相似文献   

20.
Oscillations of the line-of-sight velocities with periods 82m.2 and 76m.7 were detected in quiescent prominences, with coordinates ? = -75° W and ?= -18° W, respectively.  相似文献   

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