UDP on port 5876 thinks that error checking and correction is not necessary or performed in the application, avoiding the overhead of such processing at the network interface level. UDP (User Datagram Protocol) is a minimal message-oriented Transport Layer protocol (protocol is documented in ...

May 9, 2018 - 5876 grams to liters: Here you can find everything about 5876 g to liters, including the formula and useful information. In particular, you can obtain 5876 g in L for any density and many substances using our converters. If you are looking for how to convert 5876 grams to L, read this post.

The He I lambda 5876/hydrogen alpha line intensity ratio in the warm ionized component of the interstellar medium is significantly less than that observed in traditional H II regions surrounding O stars. The observations, carried out in two directions at low Galactic latitude, reveal that the ...

Excludes springs designed for thermal actuation (springs in which the torsion forces are counteracted by changes in temperature) and SPRING, REINFORCING, HOSE.20210050018Guns, through 30mm53600034Coil, Flat, Leaf, and Wire Springs · Part Alternates: 4100182, 5360-01-285-5876, 01-285-5876, ...

It is likely that this emission is the HeI 5876 A line originating essentially from solar wind α-particles. The relative weakness of this emission on the latitude of the polar cleft may be a consequence of the generally low energy of the particle influx in this region.

Both the light curves and the spectral development of the nova indicate that there are two separate and distinct phases of the outburst. He I 5876 A radial velocity variations observed in the second outburst phase, between 1967 December 12 and 1968 May 13, are analysed and possible periodicities ...

January 1, 1990 - We have obtained high resolution, high S/N spectra of the He I D3 line (5876 Å) for 53 stars. Combining these data with previous measurements, we investigate correlations between the flux absorbed by D3, F_D3_, rotation and other stellar activity indicators for a set of 76 G and K dwarfs.

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We give the first results of a study in F-type MS stars using the Hei D 3 absorption feature at λ5876 Å as an indicator of stellar activity and structure. The observations were obtained with the QUB echelle spectrograph at the Cassegrain focus of the 4.2 m William Herschel telescope, and ...