Multi-wavelength pumped silica-fibre Raman amplifiers

1999 ◽  
Author(s):  
S.A.E. Lewis ◽  
S.V. Chernikov ◽  
J.R. Taylor
Keyword(s):  
Raman Amplifiers ◽  
Multi Wavelength ◽  
Silica Fibre

Triple wavelength pumped silica-fibre Raman amplifiers with 114 nm bandwidth

1999 ◽  
Vol 35 (20) ◽  
pp. 1761 ◽  
Author(s):  
S.A.E. Lewis ◽  
S.V. Chernikov ◽  
J.R. Taylor
Keyword(s):  
Raman Amplifiers ◽  
Silica Fibre

Gain and saturation characteristics of dual-wavelength-pumped silica-fibre Raman amplifiers

1999 ◽  
Vol 35 (14) ◽  
pp. 1178 ◽  
Author(s):  
S.A.E. Lewis ◽  
S.V. Chernikov ◽  
J.R. Taylor
Keyword(s):  
Dual Wavelength ◽  
Raman Amplifiers ◽  
Silica Fibre

256 QAM Digital Coherent Optical Transmission Using Raman Amplifiers

2011 ◽  
Vol E94-B (2) ◽  
pp. 417-424 ◽  
Author(s):  
Masato YOSHIDA ◽  
Seiji OKAMOTO ◽  
Tatsunori OMIYA ◽  
Keisuke KASAI ◽  
Masataka NAKAZAWA
Keyword(s):  
Optical Transmission ◽  
Raman Amplifiers

Observations for the Role of Flux rope Eruption in a Geoeffective Solar Flare

2014 ◽  
Vol 4 (2) ◽  
pp. 555-564
Author(s):  
A.M Aslam
Keyword(s):  
Solar Flare ◽  
Flux Rope ◽  
Magnetic Configuration ◽  
Solar Dynamics Observatory ◽  
Multi Wavelength ◽  
Solar Dynamics ◽  
Halo Coronal Mass Ejection ◽  
Mass Ejection ◽  
The Waves

On September 24, 2011 a solar flare of M 7.1 class was released from the Sun. The flare was observed by most of the space and ground based observatories in various wavebands. We have carried out a study of this flare to understand its causes on Sun and impact on earth. The flare was released from NOAA active region AR 11302 at 12:33 UT. Although the region had already produced many M class flares and one X- class flare before this flare, the magnetic configuration was not relaxed and still continued to evolve as seen from HMI observations. From the Solar Dynamics Observatory (SDO) multi-wavelength (131 Ã…, 171 Ã…, 304 Ã… and 1600Ã…) observations we identified that a rapidly rising flux rope triggered the flare although HMI observations revealed that magnetic configuration did not undergo a much pronounced change. The flare was associated with a halo Coronal Mass Ejection (CME) as recorded by LASCO/SOHO Observations. The flare associated CME was effective in causing an intense geomagnetic storm with minimum Dst index -103 nT. A radio burst of type II was also recorded by the WAVES/WIND. In the present study attempt is made to study the nature of coupling between solar transients and geospace.

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