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331.
M. Hackstein Ch. Fein M. Haas M. Ramolla F. Pozo Nuez A. Barr Domínguez L. Kaderhandt K. Thomsch N. Niedworok Ch. Westhues R. Chini 《Astronomische Nachrichten》2015,336(6):590-603
This paper is the second in a series describing the southern Galactic Disk Survey (GDS) performed at the Univer‐sitätssternwarte Bochum near Cerro Armazones in Chile. Haas et al. (2012, Paper I) presented the survey design and the characteristics of the observations and data. They identified ∼2200 variable stars in an area of 50 square degrees with more than 50 observations in 2011. Here we present the first complete version of the GDS covering all 268 fields with 1323 square degrees along the Galactic disk including revised data from Paper I. The individual fields were observed up to 272 times and comprise a maximum time span between September 2010 and May 2015. We detect a total of 64 151 variable sources, which are presented in a catalog including some of their properties and their light curves. A comparison with the International Variable Star Index (VSX) and All Sky Automated Survey (ASAS) indicates that 56794 of these sources are previously unknown variables. Furthermore, we present U, B, V, r ′, i ′, z ′ photometry for all sources within the GDS, resulting in a new multi‐color catalog of nearly 16×106 sources detected in at least one filter. Both the GDS and the near‐infrared VISTA Variables in the Via Lactea survey (VVV) complement each other in the overlap area of about 300 square degrees enabling future comparison studies. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
332.
333.
We evaluated the effects of ultraviolet-B(UV-B) radiation and different light conditions on the repair of UV-B-induced damage in carpospores of C hondrus ocellatus Holm(Rhodophyta) in laboratory experiments. Carpospores were treated daily with different doses of UV-B radiation for 48 days,when vertical branches had formed in all treatments; after each daily treatment,the carpospores were subjected to photosynthetically active radiation(PAR),darkness,red light,or blue light during a 2-h repair stage. Carpospore diameters were measured every 4 days. We measured the growth and cellular contents of cyclobutane pyrimidine dimers(CPDs),chlorophyll a,phycoerythrin,and UV-B-absorbing mycosporine-like amino acids(MAAs) in carpospores on Day 48. Low doses of UV-B radiation(36 and 72 J/m 2) accelerated the growth of C. ocellatus. However,as the amount of UV-B radiation increased,the growth rate decreased and morphological changes occurred. UV-B radiation significant damaged DNA and photosynthetic pigments and induced three kind of MAAs,palythine,asterina-330,and shinorine. PAR conditions were best for repairing UV-B-induced damage. Darkness promoted the activity of the DNA darkrepair mechanism. Red light enhanced phycoerythrin synthesis but inhibited light repair of DNA. Although blue light,increased the activity of DNA photolyase,greatly improving remediation efficiency,the growth and development of C. ocellatus carpospores were slower than in other light treatments. 相似文献
334.
一元线性回归是应用最为广泛的参数估计方法之一。文中提出一元线性回归的自变量在等差级数的基础上进行双向黄金分割,提高两端点观测值的多余观测分量,缩小观测值之间多余观测分量的差异,在不增加观测值数量和不改变观测值精度的前提下,提高稳健估计方法消除或减弱粗差的能力。 相似文献
335.
Rémi Fahed Anthony F. J. Moffat Alceste Z. Bonanos 《Monthly notices of the Royal Astronomical Society》2009,392(1):376-382
Do some Wolf–Rayet stars owe their strong winds to something else besides radiation pressure? The answer to this question is still not entirely obvious, especially in certain Wolf–Rayet subclasses, mainly WN8 and WC9. Both of these types of Wolf–Rayet stars are thought to be highly variable, as suggested by observations, possibly due to pulsations. However, only the WN8 stars have so far been vigorously and systematically investigated for variability. We present here the results of a systematic survey during three consecutive weeks of 19 Galactic WC9 stars and one WC8 star for photometric variability in two optical bands, V and I . Of particular interest are the correlated variations in brightness and colour index in the context of carbon dust formation, which occurs frequently in WC9 and some WC8 stars. In the most variable case, WR76, we used this information to derive a typical dust grain size of ∼ 0.1 μm . However, most photometric variations occur at surprisingly low levels, and in fact almost half of our sample shows no significant variability at all above the instrumental level ( σ∼ 0.005– 0.01 mag). 相似文献
336.
B. Arbutina 《Monthly notices of the Royal Astronomical Society》2009,394(1):501-509
When the total angular momentum of a binary system is at a critical (minimum) value, a tidal instability occurs (Darwin's instability), eventually forcing the stars to merge into a single, rapidly rotating object. The instability sets in at some critical separation which in the case of contact binaries corresponds to a minimum mass ratio depending on dimensionless gyration radius k 1 . If one considers n = 3 polytrope (fully radiative primary with Γ1 = 4/3 ), k 2 1 = 0.075 and q min ≈ 0.085–0.095 . There appears to be, however, some W UMa-type binaries with q values very close, if not below these theoretical limits, implying that primary in these systems is probably more centrally condensed. We try to solve the discrepancy between theory and observations by considering rotating polytropes. We show by deriving and solving a modified Lane–Emden equation for n = 3 polytrope that including the effects of rotation does increase the central concentration and could reduce q min to as low as 0.070–0.074, more consistent with the observed population. 相似文献
337.
M. M. Montgomery 《Monthly notices of the Royal Astronomical Society》2009,394(4):1897-1907
Using smoothed particle hydrodynamics, we numerically simulate steady-state accretion discs for cataclysmic variable dwarf novae systems that have a secondary-to-primary mass ratio 0.35 ≤ q ≤ 0.55 . After these accretion discs have come to quasi-equilibrium, we rotate each disc out of the orbital plane by δ= (1, 2, 3, 4, 5 or 20)° to induce negative superhumps. For accretion discs tilted 5° , we generate light curves and associated Fourier transforms for an atlas on negative superhumps and retrograde precession. Our simulation results suggest that accretion discs need to be tilted more than 3° for negative superhumps to be statistically significant. We also show that if the disc is tilted enough such that the gas stream strikes a disc face, then a dense cooling ring is generated near the radius of impact.
In addition to the atlas, we study these artificially tilted accretion discs to find the source to negative superhumps. Our results suggest that the source is additional light from innermost disc annuli, and this additional light waxes and wanes with the amount of gas stream overflow received as the secondary orbits. The nodes, where the gas stream transitions from flowing over to under the disc rim (and vice versa), precess in the retrograde direction. 相似文献
In addition to the atlas, we study these artificially tilted accretion discs to find the source to negative superhumps. Our results suggest that the source is additional light from innermost disc annuli, and this additional light waxes and wanes with the amount of gas stream overflow received as the secondary orbits. The nodes, where the gas stream transitions from flowing over to under the disc rim (and vice versa), precess in the retrograde direction. 相似文献
338.
Gavin Ramsay Simon Rosen Pasi Hakala Thomas Barclay 《Monthly notices of the Royal Astronomical Society》2009,395(1):416-421
We report the discovery of an eclipsing polar, 2XMMi J225036.9+573154, using XMM–Newton . It was discovered by searching the light curves in the 2XMMi catalogue for objects showing X-ray variability. Its X-ray light curve shows a total eclipse of the white dwarf by the secondary star every 174 min. An extended pre-eclipse absorption dip is observed in soft X-rays at φ= 0.8–0.9 , with evidence for a further dip in the soft X-ray light curve at φ∼ 0.4 . Further, X-rays are seen from all orbital phases (apart from the eclipse) which make it unusual amongst eclipsing polars. We have identified the optical counterpart, which is faint ( r = 21) , and shows a deep eclipse (>3.5 mag in white light). Its X-ray spectrum does not show a distinct soft X-ray component which is seen in many, but not all, polars. Its optical spectrum shows Hα in emission for a fraction of the orbital period. 相似文献
339.
A. K. Dambis 《Monthly notices of the Royal Astronomical Society》2009,396(1):553-569
We use accurate absolute proper motions and Two-Micron All-Sky Survey Ks -band apparent magnitudes for 364 Galactic RR Lyrae variables to determine the kinematical parameters of the Galactic RR Lyrae population and constrain the zero-point of the Ks -band period–luminosity relation for these stars via statistical parallax. We find the mean velocities of the halo- and thick-disc RR Lyrae populations in the solar neighbourhood to be [ U 0 (Halo), V 0 (Halo), W 0 (Halo)]= (−12 ± 10, −217 ± 9, −6 ± 6) km s−1 and [ U 0 (Disc), V 0 (Disc), W 0 (Disc)]= (−15 ± 7, −44 ± 7, −25 ± 5) km s−1 , respectively, and the corresponding components of the velocity-dispersion ellipsoids, [σ VR (Halo), σ V θ (Halo), σ W (Halo)]= (167 ± 9, 86 ± 6, 78 ± 5) km s−1 and [σ VR (Disc), σ V θ (Disc), σ W (Disc)]= (55 ± 7, 44 ± 6, 30 ± 4) km s−1 , respectively. The fraction of thick-disc stars is estimated at 0.25 ± 0.03 . The corrected infrared period–luminosity relation is , implying a Large Magellanic Cloud (LMC) distance modulus of 18.27 ± 0.08 and a solar Galactocentric distance of 7.58 ± 0.40 kpc . Our results suggest no or slightly prograde rotation for the population of halo RR Lyraes in the Milky Way. 相似文献
340.
D. G. Turner †‡ D. Forbes † P. J. T. Leonard M. Abdel-Sabour Abdel-Latif D. J. Majaess L. N. Berdnikov ‡ 《Monthly notices of the Royal Astronomical Society》2009,397(2):1046-1052
Photoelectric UBV photometry and star counts are presented for the previously unstudied open cluster Collinder 236, supplemented by observations for stars near the Cepheid WZ Car. Collinder 236 is typical of groups associated with Cepheids, with an evolutionary age of (3.2 ± 1.1) × 107 yr , but it is 1944 ± 71 pc distant, only half the predicted distance to WZ Car. The cluster is reddened by E ( B − V ) ≃ 0.26 , and has nuclear and coronal radii of r n ≃ 2 arcmin (1.1 pc) and R c ≃ 8 arcmin (4.5 pc) , respectively. The Cepheid is not a member of Collinder 236 on the basis of location beyond the cluster tidal radius and implied distance, but its space reddening can be established as E ( B − V ) = 0.268 ± 0.006 s.e. from five adjacent stars. Period changes in WZ Car studied with the aid of archival data are revised. The period of WZ Car is increasing, its rate of +8.27 ± 0.19 s yr−1 being consistent with a third crossing of the instability strip. 相似文献