ALGOL

As a practical point, any computer code has to be transferable between platforms, so there is little point writing code in esoteric but obsolete languages such as French ALGOL. 

Algobblau, n. algol blue. farbe, /., farbstoff, m. algol dye. -fot, n. algol red. 

Other familiar languages may be C, ADA, LISP, ALGOL, PL/I, Prolog, and APL which are now available on many microcomputer systems. 

Pfister CA, Hay ME (1988) Associational plant refuges convergent patterns in marine and terrestrial communities result from differing mechanisms. Oecologia 77 118-129 Piazzi L, Balestri E, Cinelli F (1994) Presence of Caulerpa racemosa in the north-western Mediterranean. Cryptogam Algol 15 183-189... 

Northwest Fisheries Science Center, Harmful Algol Blooms Program. http //www.nwEc.noaa.aov/hab/index.html... 

Significantly, Balachandran, Lambert, Tomkin, and Parthasarathy (1986) have recently established that the spectrum of f3 Lyrae itself reveals the presence of CNO-cycle products. Its spectral type is too late for ready morphological detection of CNO anomalies in the blue-violet, but the quantitative analysis has shown that it is physically related to the BN binaries. Furthermore, Peters and Polidan (1984) have found evidence for extreme carbon deficiency in the high-temperature accreting material of a number of Algol-type binary systems. Hence it may be that not only are all OBN objects mass-transfer binaries, but many other mass-transfer binaries are related to the OBN category. 

The same authors (Parthasarathy et al. 1983) undertook also to examining the C and N abundances in the secondaries of the same two Algol systems, with application of the spetrum synthesis method. The result obtained suggests that in the two cases the late-type mass-losing components are carbon-deficient, Ip/Fej i-0.5, and nitrogen-rich,[N/FeJ v+0.5. 

As it is well known and has been pointed out in a recent review paper (Sahade 1986), all the ultraviolet spectra of close binary systems - except Algols - are characterized by the presence of high temperature resonance doublets of C IV, Si IV and N V, normally in emission, the ions being listed in order of decreasing intensity. 

In the Algols observed outside of eclipse, however, the resonance doublet line appear in absorption and, contrary to what we have described for the rest of the close binary systems, C IV is the weakest of the ions. This fact prompted Peters and Polidan (1984) to advance the idea that in the atmosphere of the more massive components in Algol systems, C is underabundant and N overabundant, in confirmation of Parathasarathy et al s (1983) results. 

It was interesting that a few Algols, namely, U Cep (Plavec 1983), RW Tauri (Plavec and Dobias 1983) and TT Hydrae, U Sge and UX Monocerotis (Plavec et al. 1984) were observed with the IUE satellite at principal eclipse. And on these images the resonance doublets of C IV, Si IV and N V are displayed in emission and, as far as intensities and sequence of intensities go, they behave like in the rest of the close binary systems, that is, C IV is the strongest feature of the three. 

The preceding invited paper by Sahade (1987) gave a balanced overall picture for the subject matter. I shall attempt to complement his talk in discussing two classes of atmospheric diagnostics of the evolutionary processes in interacting binary systems. These are (I) Abnormal abundances of elements in the atmosphere resulting from the nuclear processes in the stellar interior. (II) Mass flow as a consequence of the evolution of either of the components and the Algol type binaries. 

However, the physical causes of the metallic overabundances in those stars are still unclear. We shall in the following examine Algol type binaries for abundance anomalies. 

The very existence of the Algol-type binaries, in which the less massive late type component is the more evolved of the two stars, is strong evidence of the past mass loss from the late-type star as a result of its evolution. Presumably, the present late-type star was originally the more massive (component A) of the two and thus evolved off the main-sequence before its initially less massive companion (component B) did so. 

Recent observations of Algol type binaries observed in the ultraviolet, in particular with the IUE satellite, show that some form of mass flow is occurring in virtually all of them (McCluskey and Sahade 1987). 

U Cephei (V = 6.8-9.0, P = 2.493 d) is an eclipsing binary consisting of a B7V primary and a G8DI-IV secondary component. This binary is one of the semidetached Algol systems showing soft X-ray emission which is probably associated with a hot corona surrounding the secondary component (White and Marshall 1983). 

The evolution of the carbon abundance at the surface of both components of a mass-exchanging (Algol-type) binary is examined (fig. 1). Distinction is made between case B and case AB (fig. 2) of mass transfer, in view of the different timescales involved. In the mass accreting component thermohaline mixing is adopted when matter with decreasing hydrogen abundance is deposited on the surface. 

It is shown that at the surface of the loser a very low C-abundance is present, while at the surface of the gainer different regimes occur. On the average the expected C-abundance on the gainer is clearly lower than the observed solar value, but far above the value at the surface of the loser. The variation in rime during the mass-exchange process is compared to the values, derived from observation of several Algol-type systems. 

Funds available for hardware for one year were about 11,000. This limited the size of our basic system and made the requirement for modularity especially important. We plan to expand our system to increase the number of detectors that may be sampled simultaneously and increase the complexity of data reduction calculations. The expansion of core size to permit the use of Fortran or Algol would also be desirable at some future date. 

Preparation 397.—Algol Yellow R (1 5-Di-(benzoylamino)-anthra-quinone). 

Algole red 5 G and scarlet G, algole pink R. ciba red G and scarlet G, ciba Bordeaux B, helindone red B and 3 B, helindone scarlet S. helindone fast scarlet R, thioindlgo red B, thioindigo scarlet, 0 vat red. 

Algole red B. indanthrene red. indanthrene claret, ciba scarlet G... 

Indanthrene maroon, algole brown, leucole browns, dbanone brown, paramine brown ( pheaytene diamine oxidised on fibre). 

Reinsch, C. H. Numerische Mathematik 10, 177 (1967) one chapter in Sauer, R., Szabo, I. Mathematische Hilfsmittel f. Ingenieure , Springer-Verlag, Heidelberg 1970, where also ALGOL-programs can be found... 

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