Determination of the EAS cascade-curve shape by the radio method

2003 ◽  
Vol 48 (3) ◽  
pp. 112-115
Author(s):  
V. A. Tsarev ◽  
V. A. Chechin
Keyword(s):  
Curve Shape ◽  
Cascade Curve ◽  
Radio Method

Thermoluminescence Techniques in Determination of the Stress and Crystallization History of Ice

1963 ◽  
Vol 4 (34) ◽  
pp. 453-460
Author(s):  
E. J. Zeller ◽  
L. B. Ronca
Keyword(s):  
Air Temperature ◽  
Glow Curve ◽  
General Nature ◽  
Curve Shape ◽  
Shearing Stress ◽  
Sample Container ◽  
Ice Cap ◽  
History Of ◽  
High Shearing

AbstractA series of glow-curve measurements were made to determine the general nature of the thermoluminescence of natural ice. The curves were made by subjecting the samples to ultraviolet radiation from a quartz-envelope mercury arc lamp while keeping the samples at liquid air temperature. The samples were then heated by passing a stream of air over the sample container. The resultant rise in temperature is non-linear but is nearly uniform from run to run. The light emitted was measured by the microphotometric portion of the standard apparatus for determination of mineral thermoluminescence.Curves were obtained on samples collected from the ice tunnel in the ice cap at Jungfraujoch and from freshly fallen and old snow at Bern in Switzerland. A systematic variation in glow-curve shape was found. This variation appears to be directly related to the stress history of the ice. Ice which has been subjected to high shearing stress can he readily distinguished from ice which has not.

scholarly journals Properties of CVSO 30 from TESS measurements: probably a binary T Tauri star with complex light curves and no obvious planets

2020 ◽  
Vol 494 (3) ◽  
pp. 4349-4356
Author(s):  
C Koen
Keyword(s):  
Light Curve ◽  
Small Group ◽  
T Tauri Stars ◽  
Light Curves ◽  
Tauri Star ◽  
Curve Shape ◽  
T Tauri

ABSTRACT ‘Transiting Exoplanet Survey Satellite’ (TESS) photometry of CVSO 30 spanned 21.8 d, with a single large gap of 1.1 d. This allows alias-free determination of the two periodicities in the data. It is confirmed that both of these are non-sinusoidal: the dominant P1 = 0.4990 d has two detectable harmonics and P2 = 0.4486 d has seven. The large number of harmonics in the second periodicity characterizes a very complex light curve shape. One of the features in the light curve is a sharp dip of duration ∼2 h: this is probably the source of the previously claimed planetary transit signature. The star is a member of a small group of T Tauri stars with complex light curves, which have recently been exhaustively studied using Kepler and TESS observations. The two non-commensurate periods are most simply interpreted as being from two stars, i.e. CVSO 30 is probably a binary.

Determination of the cascade-curve maximum depth from the muon component on the Yakutsk EAS array

2014 ◽  
Vol 119 (5) ◽  
pp. 848-853 ◽  
Author(s):  
A. V. Glushkov ◽  
A. V. Saburov
Keyword(s):  
Maximum Depth ◽  
Muon Component ◽  
Cascade Curve ◽  
Curve Maximum

Thermoluminescence Techniques in Determination of the Stress and Crystallization History of Ice

1963 ◽  
Vol 4 (34) ◽  
pp. 453-460 ◽  
Author(s):  
E. J. Zeller ◽  
L. B. Ronca
Keyword(s):  
Air Temperature ◽  
Glow Curve ◽  
General Nature ◽  
Curve Shape ◽  
Shearing Stress ◽  
Sample Container ◽  
Ice Cap ◽  
History Of ◽  
High Shearing

Abstract A series of glow-curve measurements were made to determine the general nature of the thermoluminescence of natural ice. The curves were made by subjecting the samples to ultraviolet radiation from a quartz-envelope mercury arc lamp while keeping the samples at liquid air temperature. The samples were then heated by passing a stream of air over the sample container. The resultant rise in temperature is non-linear but is nearly uniform from run to run. The light emitted was measured by the microphotometric portion of the standard apparatus for determination of mineral thermoluminescence. Curves were obtained on samples collected from the ice tunnel in the ice cap at Jungfraujoch and from freshly fallen and old snow at Bern in Switzerland. A systematic variation in glow-curve shape was found. This variation appears to be directly related to the stress history of the ice. Ice which has been subjected to high shearing stress can he readily distinguished from ice which has not.

Determination of gamma dose and thermal neutron fluence in BNCT beams from the TLD-700 glow curve shape

2010 ◽  
Vol 45 (3-6) ◽  
pp. 640-642 ◽  
Author(s):  
G. Gambarini ◽  
G. Bartesaghi ◽  
S. Agosteo ◽  
E. Vanossi ◽  
M. Carrara ◽  
...  
Keyword(s):  
Thermal Neutron ◽  
Glow Curve ◽  
Neutron Fluence ◽  
Gamma Dose ◽  
Curve Shape

The determination of the location and frequency of thunderstorms by a radio method

1943 ◽  
Vol 69 (298) ◽  
pp. 33-44 ◽  
Author(s):  
J. S. Forrest
Keyword(s):  
Radio Method

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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