Studies on the equatorial spot of G-type contact binary UV Lyn

2021 ◽  
Author(s):  
Jingjing Wang ◽  
Bin Zhang ◽  
Linqiao Jiang
Keyword(s):  
Magnetic Activity ◽  
The Past ◽  
Photometric Observations ◽  
Massive Component ◽  
Type Contact ◽  
Contact Binary ◽  
Periodic Trend ◽  
Short Time ◽  
First Time ◽  
Magnitude Difference

Abstract New CCD photometric observations of G-type contact binary UV Lyn were obtained in 2006 and 2020, when the light curves (LCs) show positive O'Connell effect and negative O'Connell effect, especially. From the previous studies, the LCs by other ground-based telescope are variable from 1973 to 2020, particularly the magnitude difference between the two maxima. These phenomena indicate that the component is active in the past 47 years. In addition, under the monitoring of the space telescope of Transiting Exoplant Survey Satellite (TESS) from January to March in 2020, we fortunately find the continuous variations of O'Connell effect in every circle for the first time. The analysis also shows that in a short time, the positive O'Connell effect has been transformed into the negative one, which proves that there are stronger magnetic activities on the surface of the component. By using the Wilson-Devinney code with a spot model, these photometric solutions confirm UV Lyn is a shallow W-subtype contact binary with a cool equatorial spot on the less massive component. The successive variability of O'Connell effect possibly result from one equatorial cool spot shifting gradually along with time. We also investigate its \emph{O-C} curve from these continuous LCs, there is not obvious variation in such short time. while, the O’Connell effect as the indicator of the magnetic activity are possibly undergoing a periodic trend of a period of nearly 38 days. Comparing \emph{O-C} curve, we could find there is not relation between the period variation and magnetic activity.

scholarly journals The Photometric Investigation of V921 Her Using the Lunar-Based Ultraviolet Telescope of Chang’e-3 Mission

2016 ◽  
Vol 2016 ◽  
pp. 1-6 ◽  
Author(s):  
Xiao Zhou ◽  
Sheng-Bang Qian ◽  
Jia Zhang ◽  
Lin-Jia Li ◽  
Qi-Shan Wang
Keyword(s):  
Binary System ◽  
Thermal Contact ◽  
Primary Star ◽  
Light Minimum ◽  
Evolutionary Scenario ◽  
Total Luminosity ◽  
Massive Component ◽  
Contact Binary ◽  
Photometric Investigation ◽  
First Time

The light curve of V921 Her in ultraviolet band observed by the Lunar-based Ultraviolet Telescope (LUT) is analyzed by the Wilson-Devinney code. Our solutions conclude that V921 Her is an early type marginal contact binary system with an additional close-in component. The binary system is under poor thermal contact with a temperature difference of nearly 700 K between the two components. The close-in component contributes about 19% of the total luminosity in the triple system. Combining the radial velocity study together with our photometric solutions, the mass of the primary star and secondary one is calculated to beM1=1.784  (±0.055)M⊙,M2=0.403  (±0.012)M⊙. The evolutionary scenario of V921 Her is discussed. All times of light minimum of V921 Her available in the bibliography are taken into account and theO-Ccurve is analyzed for the first time. The most probable fitting results are discussed in the paper, which also confirm the existence of a third component (P3=10.2year) around the binary system. The period of V921 Her is also undergoing a continuously rapid increase at a rate ofdP/dt=+2.79×10-7  day·year-1, which may be due to mass transfer from the less massive component to the more massive one.

scholarly journals CryptoKitties Transaction Network Analysis: The Rise and Fall of the First Blockchain Game Mania

2021 ◽  
Vol 9 ◽  
Author(s):  
Xin-Jian Jiang ◽  
Xiao Fan Liu
Keyword(s):  
Network Analysis ◽  
Game Design ◽  
Rapid Decline ◽  
Public Attention ◽  
The Past ◽  
Ownership Transfer ◽  
Time In Literature ◽  
The Rich ◽  
Short Time ◽  
First Time

CryptoKitties was the first widely recognized blockchain game. Players could own, breed, and trade kitties, which are the only prop in the game. The game gained explosive growth upon its release but quickly collapsed in a short time. This study analyzes its entire player activity history for the first time in literature and tries to find the reasons for the rise and fall of this first blockchain game mania. First, we extracted the five million transaction records among 100 thousand addresses involved in CryptoKitties in the past three years. Based on the numbers of addresses involved in the game each day, we divide the game progress into four stages: the primer, the rise, the fall, and the serenity. We construct a temporal kitty ownership transfer network and analyze the varying network parameters in the four stages. We find that a large number of players poured in during the 10th and 18th days since the game release and quickly exited in the following month. Since then, a few big players have gradually dominated the game, concentrating the game resources. Through further analysis, we find that the main reason for the rapid increase in the game popularity was the increase of public attention by media outlets, while the reasons for the rapid decline in the game popularity include the oversupply of kitties, the decreasing of player income, a widening gap between the rich and poor players, and the limitations of blockchain systems. Based on these observations, we advise on the further blockchain game design: (1) to finely control the production of props and avoid an oversupply, (2) to balance the gaming cost and revenue and protect the enjoyment of players, (3) to narrow down the gap between rich and poor and create an equal gaming community, (4) to consider the limitations of blockchain systems in their game designs.

scholarly journals V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System

2022 ◽  
Vol 924 (1) ◽  
pp. 30
Author(s):  
F.-X. Li ◽  
W.-P. Liao ◽  
S.-B. Qian ◽  
E. Fernández Lajús ◽  
J. Zhang ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Triple System ◽  
Continuous Light ◽  
Close Binary ◽  
Massive Component ◽  
Cyclic Oscillation ◽  
Contact Binary ◽  
Period Decrease ◽  
First Time ◽  
Linear Period

Abstract V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O − C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O − C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = −2.08 × 10−7 days yr−1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O − C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M ⊙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.

scholarly journals Structure and evolution of W UMa-type systems

2008 ◽  
Vol 4 (S252) ◽  
pp. 423-424 ◽  
Author(s):  
Lifang Li ◽  
Fenghui Zhang ◽  
Zhanwen Han ◽  
Dengkai Jiang ◽  
Tianyu Jiang
Keyword(s):  
Binary Stars ◽  
Type Systems ◽  
Magnetic Activity ◽  
Activity Level ◽  
Average Lifetime ◽  
Type Contact ◽  
Contact Binaries ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Low Mass

AbstractWe summarize and discuss our recent works on the structure and evolution of low-mass W UMa-type contact binary stars. Three conclusions are given as followings: (1) The energy transfer is taken place in the radiative region of common envelope of W UMa systems; (2) The magnetic activity level of W UMa systems is weaker than that of non-contact binaries or rapid-rotating single stars; (3) The evolutionary outcome of W UMa systems might be the rapid-rotating single stars, and an average lifetime is derived to be about 7 Gyr for W UMa systems.

scholarly journals Ultraviolet and optical observations of the mass-losing contact binary SV Centauri

1981 ◽  
Vol 59 ◽  
pp. 487-489
Author(s):  
H. Drechsel ◽  
H.D. Radecke ◽  
J. Rahe ◽  
G. Rupprecht ◽  
W. Wargau ◽  
...  
Keyword(s):  
Mass Loss ◽  
Optical Observations ◽  
High Dispersion ◽  
Early Type ◽  
Orbital Parameters ◽  
Ultraviolet Range ◽  
Period Variations ◽  
Massive Component ◽  
Type Contact ◽  
Contact Binary

SV Cen is a well known early-type contact binary. The less massive component is a slightly evolved B1 star. The secondary is of spectral type B4 III. The period of the system is P = 1.6585 days. SV Cen shows with Ṗ/P = -2 10-5 yr-1 one of the largest known period decreases. We carried out ground-based photoelectric and spectroscopic (coudé) observations at ESO, and high dispersion UV observations at VILSPA, with the aima) to derive new orbital parameters of SV Cenb) to determine further epochs of minima (i.e. to study the period variations)c) to look for possible mass loss indicators in the ultraviolet range.

World Economy: Prospects and Barriers for Recovery

2012 ◽  
pp. 61-83 ◽  
Author(s):  
M. Ershov
Keyword(s):  
World Economy ◽  
Western World ◽  
Short Time Period ◽  
Market Segments ◽  
Junk Bonds ◽  
The Past ◽  
Time Period ◽  
The Us ◽  
Global Liquidity ◽  
Short Time

According to the latest forecasts, it will take 10 years for the world economy to get back to “decent shape”. Some more critical estimates suggest that the whole western world will have a “colossal mess” within the next 5–10 years. Regulators of some major countries significantly and over a short time‑period changed their forecasts for the worse which means that uncertainty in the outlook for the future persists. Indeed, the intensive anti‑crisis measures have reduced the severity of the past problems, however the problems themselves have not disappeared. Moreover, some of them have become more intense — the eurocrisis, excessive debts, global liquidity glut against the backdrop of its deficit in some of market segments. As was the case prior to the crisis, derivatives and high‑risk operations with “junk” bonds grow; budget problems — “fiscal cliff” in the US — and other problems worsen. All of the above forces the regulators to take unprecedented (in their scope and nature) steps. Will they be able to tackle the problems which emerge?

scholarly journals On the Short Time Scale Evolutionary History of the Contact Binary VW Cephei

1998 ◽  
Vol 11 (1) ◽  
pp. 396-396
Author(s):  
I. Pustylnik
Keyword(s):  
Evolutionary History ◽  
Light Curves ◽  
Published Data ◽  
Short Time Scale ◽  
Flare Activity ◽  
Considerable Portion ◽  
History Of ◽  
Contact Binary ◽  
Elongation Phase ◽  
Short Time

We study the short-time evolutionary history of the well-known contact binary VW Cep. Our analysis is based partly on the numerous UBV lightcurves obtained at Tartu Observatory, IUE spectra, and samples from the published data. Special attention is given to the effects of asymmetry of the light curves. A higher degree of asymmetry outside the eclipses along with the significant displacements of the brightness maxima in respect to the elongation phase is interpreted as evidence that a considerable portion of the flaring source is concentrated close to the neck connecting the components. We discuss the nature of asymmetry in terms of possible mass exchange and the flare activity and compare the results of our model computations with the record of orbital period variations over the last 60 years.

scholarly journals Efficacy of compressed sodium chloride (CSC) against E. coli and Candida auris in minutes and methods improvement for testing

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Lan N. Truong ◽  
Brayden D. Whitlock
Keyword(s):  
Sodium Chloride ◽  
Improved Method ◽  
Candida Auris ◽  
Antimicrobial Surfaces ◽  
E Coli ◽  
Route Of Transmission ◽  
The World ◽  
Short Time ◽  
First Time ◽  
Time Point

AbstractControlling infections has become one of the biggest problems in the world, whether measured in lives lost or money spent. This is worsening as pathogens continue becoming resistant to therapeutics. Antimicrobial surfaces are one strategy being investigated in an attempt to decrease the spread of infections through the most common route of transmission: surfaces, including hands. Regulators have chosen two hours as the time point at which efficacy should be measured. The objectives of this study were to characterize the new antimicrobial surface compressed sodium chloride (CSC) so that its action may be understood at timepoints more relevant to real-time infection control, under two minutes; to develop a sensitive method to test efficacy at short time points; and to investigate antifungal properties for the first time. E. coli and Candida auris are added to surfaces, and the surfaces are monitored by contact plate, or by washing into collection vats. An improved method of testing antimicrobial efficacy is reported. Antimicrobial CSC achieves at least 99.9% reduction of E. coli in the first two minutes of contact, and at least 99% reduction of C. auris in one minute.

scholarly journals Bactericidal activity of three different antiseptic ophthalmic preparations as surgical prophylaxis

2021 ◽  
Author(s):  
Daniele Tognetto ◽  
Marco R. Pastore ◽  
Gian Marco Guerin ◽  
Giuliana Decorti ◽  
Martina Franzin ◽  
...  
Keyword(s):  
Antimicrobial Activity ◽  
Povidone Iodine ◽  
Bacterial Load ◽  
Viable Cells ◽  
Polyethylene Glycol 1000 ◽  
Oil Concentration ◽  
Short Time ◽  
First Time ◽  
Antiseptic Solutions

Abstract Purpose In the era of antibiotic resistance, there is an increased interest in antiseptic solutions that might represent a reliable option for ocular surface disinfection. The objective of this study is to compare for the first time three different antiseptic ophthalmic preparations to assess their in vitro antimicrobial activity. Methods The antiseptic activity of three commercial ophthalmic solutions, IODIM (povidone-iodine 0.6% in hyaluronic acid vehicle—Medivis, Catania, Italy), OZODROP (nanoemulsion with ozonated oil—concentration not specified—FBVision, Ophthalmic Pharmaceuticals, Rome, Italy), and DROPSEPT (chlorhexidine 0.02% and vitamin E 0.5% Tocopherol Polyethylene Glycol 1000 Succinate—TPGS, Sooft Italia, Montegiorgio, Italy), was tested in vitro on six reference strains by time-killing assays. Viable cells were evaluated after 1, 15, 30 min; 2, 6, and 24 h exposure by seeding 100 µl of the suspension (or appropriate dilutions) on LB agar or Sabouraud-dextrose agar. All plates were incubated at 37 °C for 24 h and evaluated by manually counting the colonies. Results IODIM solution showed a very rapid microbicidal activity: the number of viable cells for all the tested strains was under the detection limit (less than 10 CFU/ml) already after 1 min exposure, and this result was maintained at every incubation time. The rapid antimicrobial activity of povidone-iodine was not replicated when testing the other two antiseptics. Conclusions The study reports the great efficacy in reducing bacterial load in a very short time of povidone-iodine 0.6% compared with other antiseptic preparations.

scholarly journals Diva - A Small Satellite for Global Astrometry and Photometry

1998 ◽  
Vol 11 (1) ◽  
pp. 583-583
Author(s):  
S. Röser ◽  
U. Bastian ◽  
K.S. de Boer ◽  
E. Høg ◽  
E. Schilbach ◽  
...  
Keyword(s):  
High Precision ◽  
Wavelength Range ◽  
Fizeau Interferometer ◽  
Proper Motions ◽  
Small Satellite ◽  
Short Overview ◽  
Photometric Observations ◽  
Photometric Measurements ◽  
First Time ◽  
Astronomy And Astrophysics

DIVA (Double Interferometer for Visual Astrometry) is a Fizeau interferometer on a small satellite. It will perform astrometric and photometric observations of at least 4 million stars. A launch in 2002 and a minimum mission length of 24 months are aimed at. A detailed description of the experiment can be obtained from the DIVA homepage at http://www.aip.de:8080/᷉dso/diva. An overview is given by Röser et al., 1997. The limiting magnitude of DIVA is about V = 15 for spectral types earlier than M0, but drops to about V = 17.5 for stars later than M5. Table 1 gives a short overview on DIVA’s performance. DIVA will carry out a skysurvey complete to V = 12.5. For the first time this survey will comprise precise photometry in at least 8 bands in the wavelength range from 400 to 1000 nm. DIVA will improve parallaxes by a factor of 3 compared to Hipparcos; proper motions by at least a factor of 2 and, in combination with the Hipparcos observations, by a factor of 10 for Hipparcos stars. At least 30 times asmany stars as Hipparcos will be observed, and doing this DIVA will fill the gap in observations between Hipparcos and GAIA. DIVA’s combined astrometric and photometric measurements of high precision will have important impacts on astronomy and astrophysics in the next decade.

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