scholarly journals HF Radar Observation of Velocity Fields Induced by Tsunami Waves in the Kii Channel, Japan

Author(s):  
Hirofumi HINATA ◽  
Ryotaro FUJI ◽  
Satoshi FUJII ◽  
Yuiti FUJITA ◽  
Hiroshi HANADO ◽  
...  
2011 ◽  
Vol 95 (1) ◽  
pp. 268-273 ◽  
Author(s):  
Hirofumi Hinata ◽  
Satoshi Fujii ◽  
Keita Furukawa ◽  
Tomoya Kataoka ◽  
Masafumi Miyata ◽  
...  

2007 ◽  
Vol 50 (6) ◽  
pp. 1474-1481 ◽  
Author(s):  
Zi-Ping GONG ◽  
Heng-Yu KE ◽  
Zhi-Fei DONG ◽  
Xiong-Bin WU ◽  
Feng CHENG

2015 ◽  
Vol 20 (1) ◽  
pp. 55-58
Author(s):  
Yingwei Tian ◽  
Biyang Wen ◽  
Jian Tan ◽  
Zili Li

2019 ◽  
Vol 12 (1) ◽  
pp. 97 ◽  
Author(s):  
Leonardo Bagaglini ◽  
Pierpaolo Falco ◽  
Enrico Zambianchi

Submesoscale eddies play an important role in the energy transfer from the mesoscale down to the dissipative range, as well as in tracer transport. They carry inorganic matter, nutrients and biomass; in addition, they may act as pollutant conveyors. However, synoptic observations of these features need high resolution sampling, in both time and space, making their identification challenging. Therefore, HF coastal radar were and are successfully used to accurately identify, track and describe them. In this paper we tested two already existing algorithms for the automated detection of submesoscale eddies. We applied these algorithms to HF radar velocity fields measured by a network of three radar systems operating in the Gulf of Naples. Both methods showed shortcomings, due to the high non-geostrophy of the observed currents. For this reason we developed a third, novel algorithm that proved to be able to detect highly asymmetrical eddies, often not properly identified by the previous ones. We used the results of the application of this algorithm to estimate the eddy boundary profiles and the eddy spatial distribution.


1967 ◽  
Vol 28 ◽  
pp. 177-206
Author(s):  
J. B. Oke ◽  
C. A. Whitney

Pecker:The topic to be considered today is the continuous spectrum of certain stars, whose variability we attribute to a pulsation of some part of their structure. Obviously, this continuous spectrum provides a test of the pulsation theory to the extent that the continuum is completely and accurately observed and that we can analyse it to infer the structure of the star producing it. The continuum is one of the two possible spectral observations; the other is the line spectrum. It is obvious that from studies of the continuum alone, we obtain no direct information on the velocity fields in the star. We obtain information only on the thermodynamic structure of the photospheric layers of these stars–the photospheric layers being defined as those from which the observed continuum directly arises. So the problems arising in a study of the continuum are of two general kinds: completeness of observation, and adequacy of diagnostic interpretation. I will make a few comments on these, then turn the meeting over to Oke and Whitney.


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