scholarly journals Uncertainties in the Analysis of Avoa for Determination of Fracture Orientation

1998 ◽  
Vol 53 (5) ◽  
pp. 621-627 ◽  
Author(s):  
H. Houllevigue ◽  
S. Harwood ◽  
P. S. Rowbotham ◽  
I. Bush ◽  
P. R. Williamson ◽  
...  
Keyword(s):  
Fracture Orientation

Seismic determination of fracture orientation

1989 ◽  
Author(s):  
Terry W. Spencer ◽  
Heon Cheol Chi
Keyword(s):  
Fracture Orientation

Determination of critical slip surface of fractured rock slopes based on fracture orientation data

2013 ◽  
Vol 56 (5) ◽  
pp. 1248-1256 ◽  
Author(s):  
Wen Zhang ◽  
JianPing Chen ◽  
Wu Zhang ◽  
Yan Lü ◽  
YuFei Ma ◽  
...  
Keyword(s):  
Slip Surface ◽  
Fractured Rock ◽  
Rock Slopes ◽  
Critical Slip Surface ◽  
Orientation Data ◽  
Fracture Orientation

Determination of Fracture Orientation from Pressure Interference

1960 ◽  
Vol 219 (01) ◽  
pp. 301-304 ◽  
Author(s):  
Lincoln F. Elkins ◽  
Arlie M. Skov
Keyword(s):  
Fracture Orientation

Determination of Fracture Orientation by Multi-Well Interference Testing

2002 ◽  
Author(s):  
Mohamed Cherifi ◽  
Djebbar Tiab ◽  
Freddy H. Escobar
Keyword(s):  
Fracture Orientation

Galactic orbits of stars

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley
Keyword(s):  
Globular Cluster ◽  
Potential Field ◽  
High Velocity ◽  
Velocity Vector ◽  
Variable Stars ◽  
The Sun ◽  
Proper Motions ◽  
Rr Lyrae ◽  
The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

International determination of the total motion of the pole

1961 ◽  
Vol 13 ◽  
pp. 29-41
Author(s):  
Wm. Markowitz
Keyword(s):  
Secular Motion ◽  
The Future

A symposium on the future of the International Latitude Service (I. L. S.) is to be held in Helsinki in July 1960. My report for the symposium consists of two parts. Part I, denoded (Mk I) was published [1] earlier in 1960 under the title “Latitude and Longitude, and the Secular Motion of the Pole”. Part II is the present paper, denoded (Mk II).

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