排序方式: 共有64条查询结果,搜索用时 15 毫秒
31.
32.
33.
A.C. Katsiyannis S.N. Kemp D.S. Berry J. Meaburn 《Astrophysics and Space Science》2001,276(2-4):733-740
We have digitally coadded APM scans of 13 Kodak TechPan films of the SE region of the Virgo Cluster of galaxies. The ≈6.2°×6.2°field
of the R-band films combined with the resolution of ≈2 arcsec pixel- results in data-file sizes of about 222 MBytes. The 13 scanned films have been aligned, coadded, corrected for vignetting
effects and cleaned of stellar features. To illustrate the astrophysical uses of this technique, we present high-contrast
images of a sample of interacting galaxies in the field. Several very faint features (but very clearly seen in the coadded
array) – such as the interaction between IC 3481,IC 3481A and IC 3483, and NGC 4410A and B and IC 790 – have been presented
with clarity for the first time.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
34.
J. Meaburn M. F. Graham M. P. Redman 《Monthly notices of the Royal Astronomical Society》2002,337(1):327-331
A spatially unresolved velocity feature, with an approaching radial velocity of ≈100 km s−1 with respect to the systemic radial velocity, in a position–velocity array of [O iii ] 5007-Å line profiles is identified as the kinematical counterpart of a jet from the proplyd LV 5 (158–323) in the core of the Orion nebula. The only candidate in Hubble Space Telescope ( HST ) imagery for this jet appears to be a displaced, ionized knot. Also an elongated jet projects from the proplyd GMR 15 (161–307). Its receding radial velocity difference appears at ≈80 km s−1 in the same position–velocity array.
A 'standard' model for jets from young, low-mass stars invokes an accelerating, continuous flow outwards with an opening angle of a few degrees. Here an alternative explanation is suggested which may apply to some, if not all, of the proplyd jets. In this, a 'bullet' of dense material is ejected which ploughs through dense circumstellar ambient gas. The decelerating tail of material ablated from the surface of the bullet would be indistinguishable from a continuously emitted jet in current observations. 相似文献
A 'standard' model for jets from young, low-mass stars invokes an accelerating, continuous flow outwards with an opening angle of a few degrees. Here an alternative explanation is suggested which may apply to some, if not all, of the proplyd jets. In this, a 'bullet' of dense material is ejected which ploughs through dense circumstellar ambient gas. The decelerating tail of material ablated from the surface of the bullet would be indistinguishable from a continuously emitted jet in current observations. 相似文献
35.
Y. C. Joshi D. Pollacco A. Collier Cameron I. Skillen E. Simpson I. Steele R. A. Street H. C. Stempels D. J. Christian L. Hebb F. Bouchy N. P. Gibson G. Hébrard F. P. Keenan B. Loeillet J. Meaburn C. Moutou B. Smalley I. Todd R. G. West D. R. Anderson S. Bentley B. Enoch C. A. Haswell C. Hellier K. Horne J. Irwin T. A. Lister I. McDonald P. Maxted M. Mayor A. J. Norton N. Parley C. Perrier F. Pont D. Queloz R. Ryans A. M. S. Smith S. Udry P. J. Wheatley D. M. Wilson 《Monthly notices of the Royal Astronomical Society》2009,392(4):1532-1538
We report the discovery of a 7.3 M J exoplanet WASP-14b, one of the most massive transiting exoplanets observed to date. The planet orbits the 10th-magnitude F5V star USNO-B1 11118−0262485 with a period of 2.243 752 d and orbital eccentricity e = 0.09 . A simultaneous fit of the transit light curve and radial velocity measurements yields a planetary mass of 7.3 ± 0.5 M J and a radius of 1.28 ± 0.08 R J . This leads to a mean density of about 4.6 g cm−3 making it the densest transiting exoplanets yet found at an orbital period less than 3 d. We estimate this system to be at a distance of 160 ± 20 pc. Spectral analysis of the host star reveals a temperature of 6475 ± 100 K, log g = 4.07 cm s−2 and v sin i = 4.9 ± 1.0 km s−1 , and also a high lithium abundance, log N (Li) = 2.84 ± 0.05 . The stellar density, effective temperature and rotation rate suggest an age for the system of about 0.5–1.0 Gyr. 相似文献
36.
J. Meaburn 《Astrophysics and Space Science》1968,2(1):115-127
The reasons for applying scanning Fabry-Pérot interferometers to the study of faint but extensive gaseous nebulae are outlined. Three ways of increasing the luminosity-resolutin product of the Fabry-Pérot are then investigated. 相似文献
37.
J. Meaburn 《Astrophysics and Space Science》1968,1(3):278-283
A faint nebula, between the Rosette and NGC 2264, appears to be a supernova remnant. This was photographed with long exposures through narrow filters centred on the bright nebular emission lines. Interferograms were also taken. These revealed extensive regions emitting broad lines, and showed that the nebula did not have the large expansion velocity that was expected. 相似文献
38.
John Meaburn 《Astrophysics and Space Science》1975,36(2):489-493
The performance of an image-tube insect-eye Fabry-Perot spectrograph is compared to a classical Fabry-Perot monochromator when used on some topical nebular problems. 相似文献
39.
40.
A faint filamentary structure on a Southern Schmidt plate is thought to be a supernova remnant. 相似文献