A5043134418- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Astrophysics and Star Formation Studies
- Astrophysical Phenomena and Observations
- Astronomical Observations and Instrumentation
- Gamma-ray bursts and supernovae
- Astro and Planetary Science
- Pulsars and Gravitational Waves Research
- Astrophysics and Cosmic Phenomena
- Solar and Space Plasma Dynamics
- History and Developments in Astronomy
- Geophysics and Gravity Measurements
- High-pressure geophysics and materials
- Galaxies: Formation, Evolution, Phenomena
- Particle Accelerators and Free-Electron Lasers
- Atmospheric Ozone and Climate
- Spectroscopy and Laser Applications
- Laser-Plasma Interactions and Diagnostics
- Magnetic confinement fusion research
- Scientific Research and Discoveries
- Optical Systems and Laser Technology
- Calibration and Measurement Techniques
- Mechanics and Biomechanics Studies
- Material Science and Thermodynamics
- Earthquake Detection and Analysis
Nicolaus Copernicus Astronomical Center
2016-2025
Polish Academy of Sciences
2016-2025
Institut de Radioastronomie Millimétrique
2021
Spanish National Observatory
2021
Yunnan Observatories
2010
National Astronomical Observatories
2010
University of Oxford
2010
Nicolaus Copernicus University
1982-1993
WSB Merito University in Torun
1992
Max Planck Institute for Astronomy
1989
We present a new catalogue of symbiotic stars. In our list we include 188 stars as well 28 objects suspected being symbiotic. For each star, basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray radio observations. also the spectral type cool component, maximum ionization potential observed, references to finding charts, spectra, classifications recent papers discussing physical parameters nature object. Moreover, orbital photometric...
We study X-ray and variability distance of GX 339-4. derive d>7 kpc, based on recent determination the binary parameters. data from Ginga/ASM, CGRO/BATSE, RXTE/ASM, PCA HEXTE. From 1987 to 2004, 339-4 underwent 15 outbursts went through all known states black-hole binaries. also present initial stage 2004 outburst. then colour-colour colour-flux correlations. In hard state, there is a strong anticorrelation between 1.5-5 3-12 keV spectral slopes, which we explain by thermal Comptonization...
We present X-ray/γ-ray spectra of the binary GX 339–4 observed in hard state simultaneously by Ginga and CGRO OSSE during an outburst 1991 September. The X-ray are well represented a power law with photon spectral index G ≃ 1.75 Compton reflection component fluorescent Fe Kα line corresponding to solid angle optically thick, ionized medium ∼ 0.4 × 2 π. data (= 50 keV) require sharp high-energy cut-off power-law spectrum. broad-band very modelled repeated scattering thermal plasma optical...
<i>Aims. <i/>The aims of our study are to improve the orbital elements giant and derive spectroscopic orbit for white dwarf companion symbiotic system RS Oph. Spectral variations related 2006 outburst also studied.<i>Methods. <i/> We performed an analysis about seventy optical near infrared spectra Oph that were acquired between 1998 June 2008. The orbits obtained by measuring radial velocities cool component absorption lines broad H<i>α<i/> emission wings, which seem be associated with hot...
Cyg X-3 is a highly interesting accreting X-ray binary, emitting from the radio to high-energy gamma-rays. It consists of compact object wind-fed by Wolf-Rayet (WR) star, but masses components and mass-loss rate have been subject controversies. Here, we determine its masses, inclination, using our derived relationship between mass for WR stars WN type, published infrared data, relation binary period derivative (observed be >0 in X-3). Our obtained almost identical that two independent...
To shed light on the origin of magnetic symbiotic stars, we investigated system FN Sgr in detail. We searched for a reasonable formation pathway to explain its stellar and binary parameters including field accreting white dwarf. used MESA code carry out pre-CE post-CE evolution determined outcome CE assuming energy formalism. For dwarf field, adopted crystallization scenario. found that can be explained as follows. First, non-magnetic is formed through evolution. Later, during evolution,...
Abstract In this paper, I present and discuss some recent observational results which may have important implications for our understanding of late phases binary evolution.
Barium (Ba) dwarfs and CH subgiants are the less-evolved analogues of Ba giants. They F- to G-type main-sequence stars polluted with heavy elements by a binary companion when latter was on Asymptotic Giant Branch (AGB). This is now white dwarf that in most cases cannot be directly detected. We present large systematic study 60 objects classified as or subgiants. Combining radial-velocity measurements from HERMES SALT high-resolution spectra data CORAVEL CORALIE, we determine orbital...
ABSTRACT Shocks in novae outbursts are ubiquitous, but symbiotic novae, they particularly powerful, probably because of the surrounding red giant wind. The recurrent nova RS Oph is best example this phenomenon. presence shocked plasma outburst was inferred from optical spectra, and it confirmed by X‐ray observations since 1985. Since 2010, gamma‐ray observatory Fermi has proven that general site particle acceleration, producing copious flux few‐GeV range. In last 2021, gamma‐rays were not...
Context.The study of symbiotic stars is essential to understand important aspects stellar evolution in interacting binaries. Their observed population the Galaxy however poorly known, and one three orders magnitudes smaller than predicted size.
Symbiotic stars are interacting binaries with the longest orbital periods, and their multicomponent structure makes them rich astrophysical laboratories. The accretion of a high-mass-loss-rate red giant wind on to white dwarf (WD) promising Type Ia supernova (SN Ia) progenitors. Systematic surveys for new Galactic symbiotic critical identify SN progenitors (e.g. RS Oph) better estimate total population size compare against rates. Central latter objective is building complete census towards...
We consider constraints on the distance, inclination and component masses in X-ray binary GX 339--4 resulting from published works, then construct detailed evolutionary models for donor. From both considerations, assuming black-hole nature compact object (i.e., its mass $>3\rm{M}_{\odot}$), possible donor is $\approx$0.5--$1.4\rm{M}_{\odot}$, $\approx{40}^\circ$--$60^\circ$ distance $\approx$8--12\,kpc. The corresponding of $\approx$4--$11\rm{M}_{\odot}$. confirm a previous estimate that...
view Abstract Citations (69) References (38) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS On Symbiotic Stars and Type IA Supernovae Kenyon, Scott J. ; Livio, Mario Mikolajewska, Joanna Tout, Christopher A. We examine the possibility that symbiotic stars-wide binaries containing a red giant white dwarf-produce significant fraction of Ia supernovae (SN Ia). These probably cannot account for SN events if dwarf mass must evolve to Chandrasekhar limit during...
There are no known stellar-origin double black hole (BH–BH) or black-hole–neutron-star (BH–NS) systems. We argue that Cyg X-3 is a very likely BH–BH BH-NS progenitor. This Galactic X-ray binary consists of compact object, wind-fed by Wolf-Rayet (W-R) type companion. Based on comprehensive analysis observational data, it was recently argued harbors 2–4.5 M☉ (BH) and 7.5–14.2 W-R find the fate such leads to prompt (≲ 1 Myr) formation close system for high end allowed mass (MW-R ≳ 13 M☉). For...
Using the PIONIER visitor instrument that combines light of four Auxiliary Telescopes ESO's Very Large Telescope Interferometer, we precisely measure diameters several symbiotic and related stars: HD 352, 190658, V1261 Ori, ER Del, FG Ser, AG Peg. These – in range 0.6−2.3 milli-arcsec are used to assess filling factor Roche lobe mass-losing giants provide indications on nature ongoing mass transfer. We also first spectroscopic orbit based CORAVEL HERMES/Mercator observations. The system is...
Abstract If accreting white dwarfs (WDs) in binary systems are to produce type Ia supernovae (SNe Ia), they must grow nearly the Chandrasekhar mass and ignite carbon burning. Proving conclusively that a WD has grown substantially since its birth is challenging task. Slow accretion of hydrogen inevitably leads erosion, rather than growth WDs. Rapid does lead helium layer, due both decreased degeneracy inhibition mixing accreted with underlying WD. However, until recently, simulations...
We discuss three popular explanations for the nova-like eruptions observed in symbiotic binary stars and compare model predictions with recent observations. Most outbursts occur when unstable hydrogen shell burning causes a hot white dwarf to expand radius of 1–100 R⊙. This predicts long-duration, constant-luminosity phase following visual maximum, observations novae several steady-burning sources confirm this feature thermonuclear runaway calculations. At least two symbiotics erupt...
We report on results of a Target-of-Opportunity observation the X-ray transient XTE J1118+480 performed 2000 April 14-15 with Narrow Field Instruments (0.1-200 keV) BeppoSAX satellite. The measured spectrum is power law photon index ~1.7 modified by an ultrasoft excess and high-energy cutoff above ~100 keV. soft consistent blackbody temperature ~40 eV low flux, while well fitted thermal Comptonization in plasma electron ~102 keV optical depth order unity. Consistent weakness blackbody,...
We present an analysis of new and existing photometric spectroscopic observations the ongoing eruption in symbiotic star AG Pegasi, showing that this binary has evolved considerably since turn century. Recent dramatic changes both UV continuum wind from hot component allow a more detailed than previous papers. Peg is composed normal M3 giant hot, compact embedded dense, ionized nebula. The powers activity observed system, including dense photoionized region within outer atmosphere red giant....
<i>Context. <i/>R Aqr is one of the closest symbiotic binaries and only D-type system with radial velocity data suitable for orbital parameter estimation.<i>Aims. <i/>The aims our study are to derive a reliable spectroscopic orbit Mira component, establish connections between motion other phenomena exhibited by R Aqr.<i>Methods. <i/>We reanalyze revise compiled McIntosh & Rustan complemented additional velocities.<i>Results. find an eccentric () period 43.6 yr. This solution in agreement...