摘要:

AbstractThe eigenbewegungen of the galaxies prevent the existence of a radiation universe in the past, if the present mean mass density is larger than the critical value 10−30g/cm

ISSN:0004-6337    

DOI:10.1002/asna.19722940302

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractThe equations of stellar structure are derived for relativistic stellar models assuming deviations from the weak principle of equivalence. It is estimated that observable deviations from normal neutron star models will occur if the deviation constant ε exceeds 10

ISSN:0004-6337    

DOI:10.1002/asna.19722940303

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractThe optical luminosities of extragalactic objects with broad emission lines, i.e. quasi‐stellar radio sources, radio quiet quasi‐stellar objects and Seyfert galaxies are compared. At high luminosities (M<‐ 23) we find no difference in the form of the optical luminosity function for radio quiet and radio emitting objects; at low luminosities this function is growing steeply only for radio quiet objects, whereas for objects with higher radio indices it remains nearly constant belowM= ‐ 22. This may possibly be interpreted as indicating a division between the optically bright “quasars” and the less luminous objects. The quasars with the highest radio index show only a small scatter in optical luminosities and thus yield a well defined Hubb

ISSN:0004-6337    

DOI:10.1002/asna.19722940304

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractVon NGC 659, 1027, 1245, 1502, 1528, 1907, 2420, 6830, 6866, 7062 und IC 1848 werden die Streifen‐ und Kreisbahnfunktionen sowie verschiedene charakteristische Parameter abgeleitet. Die Funktionen werden dazu benutzt „die relative Dichteverteilung in dem von diesen Haufen definierten, mittleren”︁ Haufen zu ermitteln. Für das zugeordnete verallgemeinerte SCHUSTERsche Modell ergibt sich der Exponentn= 3.04. Die Konzentration der Sterne zum Zentrum ist im mittleren Haufen etwas ausgeprägter als

ISSN:0004-6337    

DOI:10.1002/asna.19722940305

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractA quasi‐static magnetic field similar to that of a large single sunspot is assumed to be embedded in a photospheric model of an Ao star. The differences of the model atmosphere within the magnetic spot relative to the photosphere are calculated by means of the equations of hydromagnetics. The differences are small for τ ≧ I but increase towards smaller τ. The spot model is more transparent in its high layers. In equal geometrical depth the thermodynamic parameters are reduced by the magnetic field. While a small spot is darker than its photospheric surroundings, a large spot appears brighter; the wavelength dependence of its excess in brightness coincides with observations. Compared with the photosphere, the Balmer lines show narrower and deeper cores in the large spot, these differences increase towards larger quantum numbers. Also these features are qualitatively confirmed by observations.An outline is given how to extend and generalize the present model calcula

ISSN:0004-6337    

DOI:10.1002/asna.19722940306

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractIn dieser 9. Zusammenstellung von Beobachtungsergebnissen der BAV werden 208 beobachtete Minima von 46 Bedeckungssternen, 71 Maxima von 21 RR Lyrae‐ und δ Cephei‐Sternen, 232 Ergebnisse von 66 Mira‐Sternen, 72 Ergebnisse von 12 RV Tauri‐Sternen und 22 Ergebnisse von 3 Unregelmäßigen und U Geminorum‐Sternen der Jahre 1969 bis 197

ISSN:0004-6337    

DOI:10.1002/asna.19722940307

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

ISSN:0004-6337    

DOI:10.1002/asna.19722940308

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

ISSN:0004-6337    

DOI:10.1002/asna.19722940309

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

摘要:

AbstractThe effect of the magnetic field trapped into the interstellar gas on the accretion by neutron stars is considered. The account of the magnetic field decreases the accretion by 2 orders.As a result of accretion the luminosity of the neutron stars is found to be ∼ 1028– 1029erg/s and so their observation as X‐ray sources is hardly pro

ISSN:0004-6337    

DOI:10.1002/asna.19722940310

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY

ISSN:0004-6337    

DOI:10.1002/asna.19722940311

出版商:WILEY‐VCH Verlag    

年代:1972

数据来源: WILEY