Around HD 97300 and HD 97048 15 far-infrared sources are found. 3 of these are not included in the IRAS Point Source Catalogue, for 8 upper limits in the IPSC we have now determined fluxes, and confused sources have been separated better. This indicates that even this nearby region of star formation cannot be studied by just inspecting the IPSC. By including (V)JHK observations the bolometric luminosities of these sources are determined: they range from 02 to 20 LO. It concerns presumably
pre-main-sequence stars ranging in (expected) spectral type from M1 to A7.
In the paper is considered a possibility of the determination of the parameters of close binaries of he type RS CVn by means of a comparison of the light curve derived from photoelectric measurements to a synthetic curve obtained on the basis of a model of a binary system. The inverse problem method based on the nonlinear least square method is used. A few test examples and a shorter analysis of the proposed method are given.
We have compared the EINSTEIN IPC observations of RS CVn binaries with different models: a two-temperature model and a "single-loop" model. As a result, we have found that in about half of the number of observations the two components of the first model are not independent. In this case the two components can be interpreted as parts of the same loop structure rather than as belonging to different coronal structures.
A method of constructing the homogenous catalogue of diffuse objects is outlined. For the present poster, SERC (i.e. blue) plates from the UK Schmidt Telescope Unit were used.
Jets of extragalactic radio sources in many cases show signs of precessional motion. This may arise when two massive compact objects are close to each other within a galaxy nucleus. The observed radio brightness distributions are modelled by slowly precessing jets, often relativistic. Interesting illustrations of their behaviour are offered by the frequency of occurrence of one-sided jets and by an explanation of the "preferential avoidance'' effect. There may be some evidence for a binary massive black hole in the nearest galaxy nucleus, the Galactic Centre.
Energetic outflows, often colliinated into two oppositely directed jets, are frequently found to be associated with new-born stars still buried in their parent molecular clouds. Millimeter wavelength
observations of molecular transitions of species such as CO have shown that the cold molecular component of the outflows has velocities up to 60 km.s^-1 with a total mass ranging between 0.01 Mq for low mass stellar sources to over 100 Mq for flows having several massive stars at their core. Optical and near infrared
observations reveal a hot (over 10^3 Kelvin) flow component exhibiting velocities in excess of 300 km s^-1. Although some jets associated with low luminosity sources, such as HH-34, exhibit a very high degree of colliination, the structure of most massive outflows is complicated, appearing "bipolar" only in low angular
resolution observations. At high resolution, many sources exhibit lumps, oscillations, or flow in more than just two directions. In this talk I will review millimeter-wave as well as some near-infrared and optical observations of this impotant phase of stellar birth.
An experience of operating the Cambridge Research Instrumentation, Inc. Electrograph at Sacramento Peak Observatory,
N.M. is described. Some comments and suggestions on further
improvement of observations with this device are given.
During the Maximum Year, preflare and preeruptive phenomena have been observed which give a new idea on the association of eruptive prominences and coronal transients. The propagation of a C IV brightening through a prominence is related to the onset of a
MHD wave. It is followed by the activation of the prominence and its eruption some two hours later. A coronal transient is observed above 1.6 Rs. It is argued that the eruption of the prominence is
the result of perturbations in the magnetic field configuration initiated by the MHD waves. The consequence would be that more generally the primary initiation of the eruption may happen up to
several hours before the rlse of the prominence.
Based on observations of the extraordinary behind-limb flare on February 16, 1984 the radio-flux time profiles at different
dm-wavelengths and dynamic spectrum corresponding
to a source height z > 200000 km above the photosphere are
compared with hard X-ray observations reported by Kane et al.
(1987). The nature of the dm-emission and implications on the
flare process are discussed. Dependíng on the emission
process estimations of relevant plasma parameters (electron
density, magnetic field) are given.