The structure of the <Emphasis Type="Italic">AD</Emphasis> diagram for the Ursa Major flow

We consider kinematic inhomogeneities (stellar groups) in the corona of the Ursa Major flow. We show that the orientation of the major axis of the error ellipse for each star is defined by its position relative to its own apex. We apply the AD-diagram method suggested by us earlier; a statistical analysis confirms the existence of stellar groups in the corona of the Ursa Major flow.     

The effect of sewage effluent on the population density and size of the clam Parvilucina tenuisculpta

Changes in the population density and size of the clam Parvilucina tenuisculpta were related to municipal waste effluent (in particular, organic nitrogen concentration) off the coast of Palos Verdes, California. Average clam size increased as sediment organic nitrogen concentration increased, but population density increased until organic nitrogen concentration reached a critical level when population density decreased dramatically. These effects were explained in terms of increased available nutrition (in the form of sediment organic nitrogen pollutants) enhancing both population and individual size growth. However, when a critical concentration of organic decomposition products was reached, population density decreased due to the toxicity of the released compounds. It is suggested that Parvilucina tenuisculpta would make a good bioindicator of organic enrichment pollution.     

Active Stage of the Symbiotic Object MWC 560, 2018-2021

Astrophysics - Several powerful outbursts have been observed during many years of observations of the symbiotic object MWC 560. The last active stage began in the autumn of 2018 and continues to...     

Rotation of the Hyades derived from Hipparcos data

Data from the Hipparcos catalog are used to study the internal kinematics of the Hyades cluster. Cluster members whose proper motions and parallaxes are known with precisions not less than 5 mas/yr and 3 mas were used. The proper motions were reduced to the cluster center. A correlation between a component of the tangential velocity and the parallax provides evidence for possible rotation of the cluster. The total velocity gradient is 0.04±0.03 km s^?1 pc^?1. The rotation axis is located perpendicular to the direction to the Hyades apex on the celestial sphere.     

Processing method of images obtained during the TESIS/CORONAS-PHOTON experiment

In January 2009, the CORONAS-PHOTON spacecraft was successfully launched. It includes a set of telescopes and spectroheliometers—TESIS—designed to image the solar corona in soft X-ray and EUV spectral ranges. Due to features of the reading system, to obtain physical information from these images, it is necessary to preprocess them, i.e., to remove the background, correct the white field, level, and clean. The paper discusses the algorithms and software developed and used for the preprocessing of images.     

The TESIS experiment on the CORONAS-PHOTON spacecraft

On February 26, 2009, the first data was obtained in the TESIS experiment on the research of the solar corona using imaging spectroscopy. The TESIS is a part of the scientific equipment of the CORONAS-PHO-TON spacecraft and is designed for imaging the solar corona in soft X-ray and extreme ultraviolet regions of the spectrum with high spatial, spectral, and temporal resolutions at altitudes from the transition region to three solar radii. The article describes the main characteristics of the instrumentation, management features, and operation modes.     

The structure of the <Emphasis Type="Italic">AD</Emphasis> diagram for the hyades cluster

The Hyades Cluster is used to analyze details of the AD-diagram method developed in our earlier works and applied to the corona of the Ursa Major stream. Hipparcos data are used to analyze the kinematics of the Hyades Cluster and determine its apex. Evidence for rotation of the cluster is presented.