F. Jablonski
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View article: The Rings of (2060) Chiron: Evidence of an Evolving System
The Rings of (2060) Chiron: Evidence of an Evolving System Open
The centaur (2060) Chiron has long been a candidate for hosting material in orbit, based on occultation and photometric and spectroscopic data. Here, we present a multichord stellar occultation observed on 2023 September 10 UT that reveals…
Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4 Open
Measuring starspot temperatures is crucial for understanding stellar magnetic activity as it affects stellar brightness variations, influences exoplanet transit measurements, and provides constraints on the physical conditions and energy t…
Starspot temperature of CoRoT-2 from multiwavelength observations with SPARC4 Open
Measuring starspot temperatures is crucial for understanding stellar magnetic activity, as it affects stellar brightness variations, influences exoplanet transit measurements, and provides constraints on the physical conditions and energy …
Spectral Energy Distribution Analysis of the Supersoft X-ray Source CAL 87: Multiwavelength Constraints Open
We analyse the spectral energy distribution (SED) of the eclipsing supersoft X-ray source CAL 87 covering wavelengths from X-rays to the near-infrared. Our study incorporates 26 data points across ultraviolet to near-infrared, sourced from…
View article: No Evidence of Intrinsic Linear Polarization in Nova Vel 2025 (V572 Vel)
No Evidence of Intrinsic Linear Polarization in Nova Vel 2025 (V572 Vel) Open
We report on polarimetric observations of V572 Vel (Nova Vel 2025) conducted on 2025 June 26th and July 21st, shortly after its nova eruption was discovered. Our measurements in the I C band revealed an average linear polarization of 1.60%…
View article: No evidence of intrinsic linear polarization in Nova Vel 2025 (V572 Vel)
No evidence of intrinsic linear polarization in Nova Vel 2025 (V572 Vel) Open
We report on polarimetric observations of V572 Vel (Nova Vel 2025) conducted on June 26th and July 21st, 2025, shortly after its nova eruption was discovered. Our measurements in the I$_C$ band revealed an average linear polarization of 1.…
View article: The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system
The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system Open
Context. Young planetary systems represent an opportunity to investigate the early stages of (exo)planetary formation because the gravitational interactions have not yet significantly changed the initial configuration of the system. Aims. …
View article: The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system
The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system Open
Young planetary systems represent an opportunity to investigate the early stages of (exo)planetary formation because the gravitational interactions have not yet significantly changed the initial configuration of the system. TOI-4562 b is a…
TESS Photometry of AM Her and AR UMa: Binary Parameters, Cyclotron Emission Modeling, and Mass Transfer Duty Cycles Open
Transiting Exoplanet Survey Satellite (TESS) photometry of the polars AM Herculis (AM Her) and AR Ursae Majoris (AR UMa) is presented, along with high-speed photometry. AM Her shows a variety of high states with frequent transitions betwee…
Revised ephemeris and orbital period derivative of the supersoft X-ray source CAL 87 based on 34 yr of observations Open
In this study, we present an analysis of over 34 yr of observational data from CAL 87, an eclipsing supersoft X-ray source. The primary aim of our study, which combines previously analysed measurements as well as unexplored publicly availa…
Revised ephemeris and orbital period derivative of the supersoft X-ray source CAL 87 based on 34 years of observations Open
In this study, we present an analysis of over 34 years of observational data from CAL 87, an eclipsing supersoft X-ray source. The primary aim of our study, which combines previously analysed measurements as well as unexplored publicly ava…
View article: The Long-term Spectral Changes of Eta Carinae: Are they Caused by a Dissipating Occulter as Indicated by cmfgen Models?
The Long-term Spectral Changes of Eta Carinae: Are they Caused by a Dissipating Occulter as Indicated by cmfgen Models? Open
Eta Carinae ( η Car) exhibits a unique set of P Cygni profiles with both broad and narrow components. Over many decades, the spectrum has changed—there has been an increase in observed continuum fluxes and a decrease in Fe ii and H i emiss…
Revisiting multiwavelength data on the supersoft X-ray source CAL 83 Open
In this study, we revisit public data on the supersoft X-ray source CAL 83 in the Large Magellanic Cloud. A significant part of our analysis is focused on XMM–Newton X-ray observations, in which updated data reduction procedures and qualit…
Revisiting multiwavelength data on the supersoft X-ray source CAL 83 Open
In this study we revisit public data on the supersoft X-ray source CAL 83 in the Large Magellanic Cloud. A significant part of our analysis is focused on XMM-Newton X-ray observations, in which updated data reduction procedures and quality…
The long-term spectral changes of eta Carinae: are they caused by a dissipating occulter as indicated by CMFGEN models? Open
Eta Carinae ($η$\,Car) exhibits a unique set of P Cygni profiles with both broad and narrow components. Over many decades, the spectrum has changed -- there has been an increase in observed continuum fluxes and a decrease in FeII and HI em…
View article: An isolated stellar-mass black hole detected through astrometric microlensing
An isolated stellar-mass black hole detected through astrometric microlensing Open
We report the first unambiguous detection and mass measurement of an isolated stellar-mass black hole (BH). We used the Hubble Space Telescope (HST) to carry out precise astrometry of the source star of the long-duration (tE ≃ 270 days), h…
View article: Search for Magnetic Accretion in SW Sextantis Systems
Search for Magnetic Accretion in SW Sextantis Systems Open
SW Sextantis systems are nova-like cataclysmic variables that have unusual spectroscopic properties, which are thought to be caused by an accretion geometry having part of the mass flux trajectory out of the orbital plane. Accretion onto a…
New insights into time-series analysis IV: panchromatic and flux-independent period finding methods Open
New time-series analysis tools are needed in disciplines as diverse as astronomy, economics, and meteorology. In particular, the increasing rate of data collection at multiple wavelengths requires new approaches able to handle these data. …
Synchrotron Intensity and Polarization Gradients: Tools to Obtain the Magnetization Level in a Turbulent Medium Open
Synchrotron intensity and polarization gradients (SIG and SPG), proposed by Lazarian et al. and Lazarian & Yuen, present a new way to recover the mean magnetic field direction in the plane of the sky. To measure the magnetization level, La…
Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey Open
The discovery and characterization of Algol eclipsing binaries (EAs) provide an opportunity to contribute for a better picture of the structure and evolution of low-mass stars. However, the cadence of most current photometric surveys hinde…
View article: Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects. II
Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects. II Open
This is the second paper of a series presenting our search for magnetic cataclysmic variables (mCVs) among candidates selected mostly from the Catalina Real-Time Transient Survey. We present the identification spectra, obtained at the SOAR…
Broadband X-ray analysis of 1E 1740.7−2942: constraints on spin, inclination, and a tentative black hole mass Open
1E 1740.7−2942 is one of the strongest hard X-ray emitters in the Galactic Centre region, believed to be a black hole in a high-mass X-ray binary system. Although extensively studied in X-rays, many aspects about the underlying nature of t…
Distinguishing circumstellar from stellar photometric variability in Eta Carinae Open
The interacting binary Eta Carinae remains one of the most enigmatic massive stars in our Galaxy despite over four centuries of observations. In this work, its light curve from the ultraviolet to the near-infrared is analysed using spatial…
New Insights into Time Series Analysis III: Setting constraints on period analysis Open
E-science of photometric data requires automatic procedures and a precise\nrecognition of periodic patterns to perform science as well as possible on\nlarge data. Analytical equations that enable us to set the best constraints to\nproperly…
HS 2231+2441: an HW Vir system composed of a low-mass white dwarf and a brown dwarf★ Open
HW Vir systems are rare evolved eclipsing binaries composed by a hot compact star and a low-mass main-sequence star in a close orbit. These systems provide a direct way to measure the fundamental properties, e.g. masses and radii, of their…
Tandem Swift and INTEGRAL Data to Revisit the Orbital and Superorbital Periods of 1E 1740.7–2942 Open
The black hole candidate 1E 1740.7−2942 is one of the strongest hard X-ray sources in the Galactic Center region. No counterparts in longer wavelengths have been identified for this object yet. The presence of characteristic timing signatu…
Multi-band characterization of the hot Jupiters: WASP-5b, WASP-44b and WASP-46b Open
We have carried out a campaign to characterize the hot Jupiters WASP-5b,\nWASP-44b and WASP-46b using multiband photometry collected at the\nObservat\\'orio do Pico Dos Dias in Brazil. We have determined the planetary\nphysical properties …
He II λ4686 EMISSION FROM THE MASSIVE BINARY SYSTEM IN η CAR: CONSTRAINTS TO THE ORBITAL ELEMENTS AND THE NATURE OF THE PERIODIC MINIMA*†‡§ Open
Eta Carinae ( η Car) is an extremely massive binary system in which rapid spectrum variations occur near periastron. Most notably, near periastron the He ii λ 4686 line increases rapidly in strength, drops to a minimum value, then increase…