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1.
On June 27, 1997, the Near Earth Asteroid Rendezvous (NEAR) spacecraft flew within 1200km of the main belt asteroid 253 Mathilde. Previous observations of Mathilde had revealed it to be a C-type asteroid with an astonishingly-long rotation period of 17.4 days, an albedo of 3.8%, and a mean diameter of 60 km. Observations by NEAR reveal that Mathilde has a roughly triaxial shape of 66 × 48 × 46 km diameter and a mass of 1. 02 × 10 g, implying a mean density of only 1. 3g/cm3 . The surface of Mathilde was observed to be saturated with large impact craters, showing a range of visible topography in excess of 5 km. Multispectral observations did not reveal any substantial color differences across the surface, and coverage at multiple phase angles was used to derive a preliminary albedo of 3. 5 % to 5% .The low observed density, lack of color variations, and low albedo all suggest that Mathilde may be a primitive, carbon - rich object with an interior that contains substantial pore space.  相似文献   

2.
GSC 4560-02157 is a new eclipsing cataclysmic variable with an orbital period of 0.265359 days.By using the published V- and R-band data together with our observations,we discovered that the O-C curve of GSC 4560-02157 may show a cyclic variation with a period of 3.51 years and an amplitude of 1.40 min.If this variation is caused by a light travel-time effect via the existence of a third body,then its mass can be derived as M_3 sin i′≈91.08 M_(Jup),and it should be a low-mass star.In addition,several physical parameters were measured.The color of the secondary star was determined to be V-R =0.77(±0.03) which corresponds to a spectral type of K2-3.The secondary star's mass was estimated as M_2 = 0.73(±0.02) M_☉ by combing the derived V-R value around phase 0 with the assumption that it obeys the mass-luminosity relation for main sequence stars.This mass is consistent with the mass-period relation for CV donor stars.For the white dwarf,the eclipse durations and contacts of the white dwarf yield an upper limit on the white dwarf's radius corresponding to a lower limit on mass of M_1≈0.501 M_☉.The overestimated radius and previously published spectral data indicate that the boundary layer may have a very high temperature.  相似文献   

3.
We characterize the morphology of the photometric phase curve model of an asteroid with a threeparameter magnitude phase function H-G_1-G_2 system by considering the effect of brightness variation arising from a triaxial ellipsoid representing the asteroid's shape.Applying this new model and a Markov Chain Monte Carlo method,we refine the photometric phase curve of asteroid(107) Camilla and obtain its absolute magnitude H=7.026_(-0.054)~(+0.052) mag,and phase function parameters G_1=0.489_(-0.044)~(+0.043) and G_2=0.259_(-0.023)~(+0.023).Meanwhile,we also determine(107) Camilla's orientation of pole(74.1°_(-4.5°)~(+4.3°),50.2°_(-5.0°)~(+5.4°)with rotational period of 4.843928_(-0.000001)~(+0.000001)h,and axial ratios a/b=1.409_(-0.020)~(+0.020) and b/c=1.249_(-0.060)~(+0.063).Furthermore,according to the values of phase function parameters G_1 and G_2,we infer that asteroid(107)Camilla is an X-type asteroid.  相似文献   

4.
1 INTRODUCTIONThe FAST is an ArecibChtype telescope with a number of innovations, which is to be built inthe unique karst area of Southwest China (Nan Rendong et al. 1996). Some basic parametersof the FAST have been tentatively suggested such as, curvature radius R = 300m, openingangle 0 = 120', and frequency range from 300MHz to 5 GHz. Baized on the fact that thecelltral part of a spherical surface deyiates little from a paraboloid as a proper focal length ischosen, a novel design…  相似文献   

5.
We have obtained deep J and Ks-band images centered on a bright radio quiet QSO UM 402(zem= 2.856) using the IRCS camera and adaptive optics systems that are part of the Subaru Telescope, as well as retrieved WFC3/F140 W archive images of this object. A faint galaxy(mk= 23.32 ± 0.05 in the Vega magnitude system)that lies ～ 2.4′′north of the QSO sightline has been clearly resolved in all three deep high resolution datasets, and appears as an irregular galaxy with two close components in the Ks-band images(separation ～ 0.3′′). Given the small impact parameter(b = 19.6 kpc, at zlls= 2.531), as well as the red color of(J- K s)Vega～ 1.6,it might be a candidate galaxy giving rise to the Lyman Limit system absorption at zabs= 2.531 seen in the QSO spectrum. After carefully subtracting the point spread function from the QSO images, the host galaxy of this bright radio quiet QSO at z ～ 3was marginally revealed. We placed a lower limit on the host component of mk～ 23.3according to our analyses.  相似文献   

6.
We investigate the radial color gradients of galactic disks using a sample of - 20 000 face-on spiral galaxies selected from the fourth data release of the Sloan Digital Sky Survey （SDSS-DR4）. We combine galaxies with similar concentrations, sizes and luminosities to construct composite galaxies, and then measure their color profiles by stacking the azimuthally averaged radial color profiles of all the member galaxies. Except for the smallest galaxies （R50 〈 3 kpc）, almost all galaxies show negative disk color gradients with mean 9 - r gradient Ggr = -0.006 magkpc-1 and r - z gradient Grz = -0.018 mag kpc^-1. The disk color gradients are independent of the morphological types of galaxies and strongly dependent on the disk surface brightness μd, with lower surface brightness galactic disks having steeper color gradients. We quantify the intrinsic correlation between color gradients and surface brightness as Ggr = -0.011μd ＋ 0.233 and Grz - -0.015μd ＋ 0.324. These quantified correlations provide tight observational constraints on the formation and evolution models of spiral galaxies.  相似文献   

7.
W UMi is a near contact, semi-detached, double-lined eclipsing binary star with an orbital period of 1.7 d. Simultaneous analysis of new BV R multi-color light curves and radial velocity data yields the main astrophysical parameters of the binary and its component stars. We determined mass and radius to be M_1 = 3.22 ± 0.08 M_⊙, R_1 = 3.63 ± 0.04 R_⊙ for the primary star and M_2 = 1.44 ± 0.05 M_⊙,R_2 = 3.09 ± 0.03 R_⊙ for the secondary star. Based on analysis of mid-eclipse times, variation in the orbital period is represented by a cyclic term and a downward parabola. Mass loss from the system is suggested for a secular decrease(-0.02 s yr~(-1)) in the period. Both the mechanisms of a hypothetical tertiary star orbiting around W UMi and the surface magnetic activity of the less massive cooler companion were used to interpret periodic changes. Observational parameters were found to be consistent with binary stellar evolution models produced in the non-conservative approach of MESA at a higher metallicity than the Sun and an age of about 400 Myr for the system. Evidence that the system is rich in metal was obtained from spectral and kinematic analysis as well as evolution models. W UMi, a high mass ratio system compared to classical semi-detached binaries, is an important example since it is estimated from binary evolutionary models that the system may reach its contact phase in a short time interval.  相似文献   

8.
We investigate the surface thermophysical properties(thermal emissivity, thermal inertia,roughness fraction and geometric albedo) of asteroid(99942) Apophis, using the currently available mid-infrared observations from CanariC am on Gran Telescopio CANARIAS and far-infrared data from PACS on Herschel, based on the Advanced Thermophysical Model. We show that the thermal emissivity of Apophis should be wavelength dependent from 8.70 μm to 160 μm, and the maximum emissivity may appear around 20 μm, similar to that of Vesta. Moreover, we further derive the thermal inertia,roughness fraction, geometric albedo and effective diameter of Apophis within a possible 1σ scale of Γ = 100_(-52)~(+100)+Jm~(-2)s~(-0.5)K~(-1), f_r = 0.78~1.0, p_v = 0.286_(-0.026)~(+0.030) and D_(eff) = 378_(-25)~(+19)m, and 3σscale of Γ = 100_(-100)~(+240)Jm~(-2)s~(-0.5) K~(-1), f_r = 0.2~1.0, p_v = 0.286_(-0.029)~(+0.039) and D_(eff) = 378_(-29)~(+27) m. The derived low thermal inertia but high roughness fraction may imply that Apophis could have regolith on its surface, where stronger space weathering but weaker regolith migration has happened in comparison with asteroid Itokawa. Our results show that small-size asteroids could also have fine regolith on the surface, and further infer that Apophis may have been delivered from the Main Belt by the Yarkovsky effect.  相似文献   

9.
In China’s asteroid mission to be launched around 2025,(7968)133 P/Elst-Pizarro(hereafter 133 P)will be the second target,after a visit to asteroid(469219)Kamo’oalewa.This paper describes a simulation of precise orbit determination for the spacecraft around comet 133 P,as well as estimation of its gravitational parameter(GM)value and the solar radiation pressure coefficient Cr for the spacecraft.Different cometocentric distances of 200,150 and 100 km orbits are considered,as well as two tracking modes:exclusive two-way range-rate mode(Earth station to spacecraft)and combinations of two-way range-rate and local spacecraft onboard ranging to the comet.Compared to exclusive two-way range-rate,the introduction of local ranging observables improves the final GM uncertainties by up to one order of magnitude.An ephemeris error in the orbit of 133 P is also considered,and we show that,to obtain a reliable estimate of the GM for 133 P,this error cannot exceed a one km range.  相似文献   

10.
As the asteroid rotational period is important to the study of the properties of asteroids(e.g.,super-fast rotators have structures owing an internal cohesion(rather than being rubble piles bounded by gravity only) so as not to fly apart), constructing an effective and fast method used to search the period attracts much researchers' attention. Recently, the Bayesian generalized Lomb–Scargle(BGLS)periodogram was developed to improve the convergence efficiency of the Lomb–Scargle method. However,the result of BGLS varies with the frequency range and cannot meet the two minimum/maximum requirements for a complete rotation of the asteroid. We propose a robust BGLS-based method that efficiently determines rotational periods. The proposed method employs a polynomial series to fit folded light curves with potential periods, initially calculated using the BGLS periodogram, and adopts a merit function to estimate and refine best-fit periods. We estimate the rotational periods of 30 asteroids applying the new method to light curves from the Palomar Transient Factory. Results confirm the effectiveness of the BGLS-based method in deriving rotational periods from ground-based observations of asteroids. Further application of the BGLS-based method to sparse light curves, such as Gaia data, is discussed.  相似文献   

11.
The cross section for a neutron-deuteron(nd) radiative capture is calculated using the pionless effective field theory including isospin symmetry breaking(ISB) corrections up to higher order.The triton is studied as a three-body bound state and one has to take into account various ISB effects,relativistic corrections and external electromagnetic currents.The isospin violation in nd radiative capture is improved compared to the one at NLO and N2LO.The cross section is determined to beσtot= [0.505 ± 0.003] mb up to N2LO.A satisfactory agreement between theory and experiment for the calculated cross section has been found by insertion of three-body forces and ISB effects.  相似文献   

12.
Currently two-way and three-way spacecraft Doppler tracking techniquesare widely used and play important roles in control and navigation of deep space mis-sions. Starting from a one-way Doppler model, we extend the theory to two-way andthree-way Doppler models by making them include possible violations of the localLorentz invariance （LLI） and the local position invariance （LPI） in order to test theEinstein equivalence principle, which is the cornerstone of general relativity and allother metric theories of gravity. After taking the finite speed of light into account,which is the so-called light time solution （LTS）, we make these models depend on thetime of reception of the signal only for practical convenience. We find that possibleviolations of LLI and LPI cannot affect two-way Doppler tracking under a linear ap-proximation of LTS, although this approximation is sufficiently good for most cases inthe solar system. We also show that, in three-way Doppler tracking, possible violationsof LLI and LPI are only associated with two stations, which suggests that it is betterto set the stations at places with significant differences in velocities and gravitationalpotentials to obtain a high level of sensitivity for the tests.  相似文献   

13.
At present, optical autonomous navigation has become a key technologyin deep space exploration programs. Recent studies focus on the problem of orbit de-termination using autonomous navigation, and the choice of filter is one of the mainissues. To prepare for a possible exploration mission to Mars, the primary emphasisof this paper is to evaluate the capability of three filters, the extended Kalman filter（EKF）, unscented Kalman filter （UKF） and weighted least-squares （WLS） algorithm,which have different initial states during the cruise phase. One initial state is assumedto have high accuracy with the support of ground tracking when autonomous navi-gation is operating; for the other state, errors are set to be large without this support.In addition, the method of selecting asteroids that can be used for navigation fromknown lists of asteroids to form a sequence is also presented in this study. The simula-tion results show that WLS and UKF should be the first choice for optical autonomousnavigation during the cruise phase to Mars.  相似文献   

14.
The kinematics of superluminal components in blazar 3C 454.3 are studied.Nine components are included： superluminal knots R1, R2, R3, R4, A, B, C and D（from Britzen et al. 2013） and C4 （from Pauliny-Toth 1998）. We find that their kine-matics derived from VLBI observations can be consistently interpreted in terms of ajet precession scenario with a period of about 14.5 yr. We discuss the model fits oftheir trajectory, distance from the core and apparent velocity. We show that the bulkLorentz factor （in the range 4 to 15） derived for these components does not have anydependence on the phase of the precession （or position angle for ejection）. The Lense-Thirring effect is assumed to interpret the precession of the jet nozzle. The resultsobtained for blazar 3C 454.3 are only suggestive. They are not unique and have yet tobe tested, but they might be useful for understanding the kinematics of superluminalcomponents in blazars and for disentangling different mechanisms and factors.  相似文献   

15.
Recent observations have found that chromospheric spicules behave likeAlfvenic fluctuations. Low-frequency Alfven waves are predicted to partially reflectin the transition region that has a gradient in the Alfven speed, thereby producinginward Alfven waves, which may interact nonlinearly with outward Alfven wavesto generate Alfv6nic turbulence. However, the signature of Alfvenic turbulence in thechromosphere has not yet been quantitatively analyzed with observations. Here we an-alyze some characteristics related to Alfv6nic turbulence with the observations fromHinode/SOT. We decompose the height-time diagram of the transverse oscillationsto separate the outward and inward propagating Alfvenic-like signals. The counter-propagating waves are found to have similar amplitude, period and phase speed, sug-gesting a state having an approximate balance in bi-directional energy fluxes. Counter-propagation of intensity oscillation with lower propagation speed is also presented,probably indicating the presence of slow mode waves. Moreover, we attempt to esti-mate the Elseisser spectra of the chromospheric turbulence for the first time. The rela-tive fluctuations in the magnetic field may be measured as the local slope of wave-likeshapes in spicules. The resulting low-frequency Elsaisser power spectra look similarto each other without showing a dominant population, which confirms these counter-propagating low-frequency Alfv6nic waves are in a state of balanced flux. These obser-vational results are believed to help us better understand the nature of chromosphericturbulence as well as chromospheric heating.  相似文献   

16.
The reduced transition probabilities from an electric quadrupole B(E2) and reduced transition probabilities from a magnetic dipole B(M1) between the ground state and the first excited state have been calculated for the3He(α,γ)7Be,8Be(α,γ)12C and12C(α,γ)16O radiative capture reactions with the M3Y potential.These reactions are important in stellar evolution.The calculated B(M1) and B(E2) for7Be nuclei are found to be 1.082×10-3e2fm2and 1.921 e2fm4from transitions 3/2-to 1/2-,respectively.The obtained values for reduced transition probabilities B(E2) for the12C and16O nuclei from transitions 0+to 2+are 12.54 e2fm4and 14.18 e2fm4,respectively.The results are in satisfactory agreement with available experimental data.  相似文献   

17.
We are developing and testing active baluns and electrically short dipoles for possible use as the primary wide band receiving elements in the low-frequency array (LOFAR) for long wavelength radio astronomy. Several dipoles of various designs and dimensions have been built and tested. Their useful range occurs when the dipole arms are approximately to one wavelength long and the feedpoint is less than wavelength above ground. An eight-element NRL LOFAR test array (NLTA) interferometer has been built and fringes have been observed from the brightest celestial sources in the frequency range from 10 to 50 MHz. The antenna temperatures vary from about 10% to 100% of the average brightness temperature of the galactic background. With these parameters it is easy to make the amplifier noise levels low enough that final system temperature is dominated by the galactic background.  相似文献   

18.
Cosmic-ray induced neutrino backgrounds at the Moon are estimated using a semi-analytic approach. The analytic expressions are derived, flux estimates for and are given, and comparisons with the analogous backgrounds generated in the Earth’s atmosphere are presented. Suppression of the lunar fluxes relative to the terrestrial fluxes is found. At energies >10 GeV, the suppression approaches a maximum of order 10−4. The lower background environment suggests that the Moon may be advantageous for future particle astrophysics endeavors.  相似文献   

19.
The different timing results of the magnetar Swift J1822.3—1606 are analyzed and understood theoretically.It is noted that different timing solutions are caused not only by timing noise,but also because the period derivative is decreasing after the outburst.Both the decreasing period derivative and the large timing noise may originate from wind braking associated with the magnetar.Future timing of Swift J1822.3—1606 will help clarify whether or not its period derivative is decreasing with time.  相似文献   

20.
Jupiter's radio emissions at frequencies below 300 MHz have never been imaged at high spatial resolution. In this paper we discuss the role of LOFAR to image Jupiter's synchrotron radiation at low frequencies to study the low-energy, barely relativistic, electron population in the planet's radiation belts. Radio spectra of Jupiter's synchrotron radiation have revealed significant modifications over time at frequencies between 100 and 1000 MHz, suggestive of processes such as pitch angle scattering by plasma waves, Coulomb scattering and perhaps energy degradation by dust. With LOFAR we may begin investigating the cause of such variability through its imaging capabilities at frequencies 200 MHz at high angular resolution. In particular, quasi-simultaneous observations with LOFAR and higher frequency arrays, such as the Very Large Array (VLA), may provide the necessary data to identify the cause of such variability, which is tightly coupled to the origin and mode of transport (including source/loss terms) of the high-energy electrons in Jupiter's inner radiation belts.  相似文献   

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