Space astrophysical observatory ?Orion-2?

Gurzadyan, G. A.; Jarakyan, A. L.; Krmoyan, M. N.; Кашин, А. Л.; Loretsyan, G. M.; Ohanesyan, J. B.

doi:10.1007/bf00640454

Cited by 6 publications

(6 citation statements)

References 7 publications

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“…When the angular dimensions of the nebula are fairly large, or the central star is weak enough, the photometric results should be meaningful to the investigation of the nebula. According to preliminary data two-photon radiation plays in such nebulae a far greater role than it was believed earlier; the impression is that almost all recombinations pass through the level 2s, or it may be that a true process of fragmentation of Lyman photons (Gurzadyan 1969), is going on in the nebulae.…”

Section: Wide-band Short-wave Photometry Of Planetary Nebulaementioning

confidence: 93%

“…4, open circles) from the measurements and processing of the f, 0rion-2 n spectrogram. Mihalas' (1965) model for an effective temperature T e ff = 50,000°K (suggested by estimates of M3,000° by Gurzadyan (1969) and 66,000°K by O'Dell (1962)) is shown in Figure 4 as the solid line.…”

Section: Continuous Spectrum Of the Central Starmentioning

confidence: 94%

“…The proposed identifications for some of these lines are given in Table I together with very approximate estimates of their relative intensities (in units E(Hg) = 10, we have Ε (Λ3727 [Oil] ) = 11); a detailed discussion of each follows. (Gurzadyan 1965;1969). The doublet itself arises from the transitions 2 Ö3/2, 5/2 k Ss/2 which are isoelectronic with À3726 + 3729 [Oil].…”

Section: Shortwave Spectra Of the Planetary Nebulaementioning

confidence: 99%

“…The difference between theory and observations is large and arises from interstellar absorption which seems to obey a λ"1 law (Gurzadyan 1975), at least down to 2500-2400 A; the divergence from this law appears around 2400 A, and reaches to a maximum at 2200 A (Bless and Savage 1972). The corrected continuous spectrum of the central star is given in Figure 4 by filled circles.…”

Section: Continuous Spectrum Of the Central Starmentioning

confidence: 99%

“…This was due to the faintness of these objects (the brightest of them barely attaining eighth magnitude) and to the difficulties in locating and tracking them from spaceship or vertical rocket. Still, upon the first serious attempt in December 1973, the ultraviolet spectrogram of IC 2149 was obtained with the help of the space observatory n 0rion-2 n installed on board the spaceship SOYUZ-13 (Gurzadyan et al 1974). Then in 1974 an Aerobee rocket took the electronographic picture of the short-wave spectrum of NGC 7027, and a little later, that of NGC 7662 (Bohlin et al 1975).…”

Section: Introductionmentioning

confidence: 99%

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Ultraviolet Observations of Planetary Nebulae

Gurzadyan¹

1978

Symp. - Int. Astron. Union

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The ultraviolet spectra of gaseous nebulae have for long been arresting the attention of astrophysicists. The 60's saw the first attempts at plotting the expected spectra of planetary nebulae between 3000 and 912 Å (Code 1960; Aller 1961). This was followed by an examination of the expected forbidden lines (about thirty of them) in the ultraviolet, and of their relation to physical parameters (Gurzadyan 1965; Osterbrock 1963). Even more accurate calculations were made for the intensities of stronger lines in highly excited nebulae (Flower 1968). At the same time preliminary estimates were being made of atomic parameters for various transitions - the collision strengths, the probabilities of forbidden transitions, etc. (Czyzak et al. 1968; Garstang 1968). The computations of various models for planetary nebulae also bear on the above studies (Harrington 1968; Kirkpatrick 1970).

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Section: Wide-band Short-wave Photometry Of Planetary Nebulaementioning

confidence: 93%

Section: Continuous Spectrum Of the Central Starmentioning

confidence: 94%

Section: Shortwave Spectra Of the Planetary Nebulaementioning

confidence: 99%

Section: Continuous Spectrum Of the Central Starmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Ultraviolet Observations of Planetary Nebulae

Gurzadyan¹

1978

Symp. - Int. Astron. Union

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Über eine lichtelektrische Nachführung als Hauptelement einer automatisierten Teleskopsteuerung (Mitteilung der Universitäts‐Sternwarte zu Jena Nr. 131)

Schielicke¹

1978

Astron Nachr

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Es wird cine automatische Teleskopnachfuhrung beschrieben, die auf der Zeitmethode basiert. Besondere Merkmale sind die Verwendung nur eines SEV, die Beriicksichtigung der Szintillation, die Mdglichkeit, den Totgang der Teleskopantriebe zu konipensieren und die digitale Arbeitsweise der Regelung, wodurch es moglich ist, ncben der beschriebenen speziellen Auswerte-und Stellelektronik auch einen Steuerrechner fur die Nachfuhrung einzusetzen. Die Nachfuhrgenauigkeit liegt in der GrdBenordnung +o:I.An autoguider based on the time-method is described. It is charactcrized by using one multiplier only, taking into account the szintillation, compensating if neccssary the backlash of the gearing. and using digital techniques. Therefore, it is possible to use for the guider the special elcctronics describcd or a control computer. The accuracy of the setting is about AoIr.

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1.4 UV and EUV instruments

Werner

2010

Landolt-Börnstein - Group VI Astronomy and Astrophysics

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Space astrophysical observatory ?Orion-2?

Cited by 6 publications

References 7 publications

Ultraviolet Observations of Planetary Nebulae

Ultraviolet Observations of Planetary Nebulae

Über eine lichtelektrische Nachführung als Hauptelement einer automatisierten Teleskopsteuerung (Mitteilung der Universitäts‐Sternwarte zu Jena Nr. 131)

1.4 UV and EUV instruments

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