| 1. |
- Alvarado-Gomez, Julian D., et al.
(författare)
-
Far beyond the Sun - I. The beating magnetic heart in Horologium
- 2018
-
Ingår i: Monthly notices of the Royal Astronomical Society. - : Oxford University Press. - 0035-8711 .- 1365-2966. ; 473:4, s. 4326-4338
-
Tidskriftsartikel (refereegranskat)abstract
- A former member of the Hyades cluster, iota Horologii (iota Hor) is a planet-hosting Sun-like star which displays the shortest coronal activity cycle known to date (P-cyc similar to 1.6 yr). With an age of similar to 625 Myr, iota Hor is also the youngest star with a detected activity cycle. The study of its magnetic properties holds the potential to provide fundamental information to understand the origin of cyclic activity and stellar magnetism in late-type stars. In this series of papers, we present the results of a comprehensive project aimed at studying the evolving magnetic field in this star and how this evolution influences its circumstellar environment. This paper summarizes the first stage of this investigation, with results from a long-term observing campaign of iota Hor using ground-based high-resolution spectropolarimetry. The analysis includes precise measurements of the magnetic activity and radial velocity of the star, and their multiple time-scales of variability. In combination with values reported in the literature, we show that the long-term chromospheric activity evolution of iota Hor follows a beating pattern, caused by the superposition of two periodic signals of similar amplitude at P-1 similar or equal to 1.97 +/- 0.02 yr and P-2 similar or equal to 1.41 +/- 0.01 yr. Additionally, using the most recent parameters for iota Hor b in combination with our activity and radial velocity measurements, we find that stellar activity dominates the radial velocity residuals, making the detection of additional planets in this system challenging. Finally, we report here the first measurements of the surface longitudinal magnetic field strength of iota Hor, which displays varying amplitudes within +/- 4G and served to estimate the rotation period of the star (P-rot = 7.70(-0.67)(+0.18) d).
|
|
| 2. |
- Kochukhov, Oleg, et al.
(författare)
-
Magnetic field topology and chemical abundance distributions of the young, rapidly rotating, chemically peculiar star HR5624
- 2017
-
Ingår i: Astronomy and Astrophysics. - : EDP SCIENCES S A. - 0004-6361 .- 1432-0746. ; 605
-
Tidskriftsartikel (refereegranskat)abstract
- Context. The young, rapidly rotating Bp star HR5624 (HD 133880) shows an unusually strong non-sinusoidal variability of its longitudinal magnetic field. This behaviour was previously interpreted as the signature of an exceptionally strong, quadrupole-dominated surface magnetic field geometry.Aims. We studied the magnetic field structure and chemical abundance distributions of HR5624 with the aim to verify the unusual quadrupolar nature of its magnetic field and to investigate correlations between the field topology and chemical spots. Methods. We analysed high-resolution, time series Stokes parameter spectra of HR5624 with the help of a magnetic Doppler imaging inversion code based on detailed polarised radiative transfer modelling of the line profiles.Results. We refined the stellar parameters, revised the rotational period, and obtained new longitudinal magnetic field measurements. Our magnetic Doppler inversions reveal that the field structure of HR5624 is considerably simpler and the field strength is much lower than proposed by previous studies. We find a maximum local field strength of 12 kG and a mean field strength of 4 kG, which is about a factor of three weaker than predicted by quadrupolar field models. Our model implies that overall large-scale field topology of HR5624 is better described as a distorted, asymmetric dipole rather than an axisymmetric quadrupole. The chemical abundance maps of Mg, Si, Ti, Cr, Fe, and Nd obtained in our study are characterised by large-scale, high-contrast abundance patterns. These structures correlate weakly with the magnetic field geometry and, in particular, show no distinct element concentrations in the horizontal field regions predicted by theoretical atomic diffusion calculations.Conclusions. We conclude that the surface magnetic field topology of HR5624 is not as unusual as previously proposed. Considering these results together with other recent magnetic mapping analyses of early-type stars suggests that predominantly quadrupolar magnetic field topologies, invoked to be present in a significant number of stars, probably do not exist in real stars. This finding agrees with an outcome of the MHD simulations of fossil field evolution in stably stratified stellar interiors.
|
|
| 3. |
- Krticka, J., et al.
(författare)
-
Testing Opacities Using the SED Variability of Chemically Peculiar Stars
- 2018
-
Ingår i: WORKSHOP ON ASTROPHYSICAL OPACITIES. - : ASTRONOMICAL SOC PACIFIC. - 9781583819142 ; , s. 195-200
-
Konferensbidrag (refereegranskat)abstract
- Opacity variations across stellar surfaces are the key process producing the spectral energy distribution (SED) variability in chemically peculiar (CP) stars. The opacity variations are caused by the presence of surface spots with enhanced (or depleted) abundances of chemical elements. Simulations of the SED variability of chemically peculiar stars with abundances derived from Doppler mapping provide a detailed test of the continuum (bound free) and line opacities in the model atmospheres. The effect of opacities on the SED is most pronounced in the ultraviolet region. We simulate the ultraviolet and visual SED variability of selected chemically peculiar stars using model atmospheres calculated for actual surface abundances, and compare the predicted SEDs with observational results. We show that the simulations can reliably predict the observed SED and its variability as long as complete bound free and bound bound opacities are used. Therefore, the variability of chemically peculiar stars may serve as a test of opacities included in model atmospheres.
|
|
| 4. |
- Krticka, J., et al.
(författare)
-
The nature of light variations in magnetic hot stars
- 2018
-
Ingår i: CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO. - : SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST. - 1335-1842. ; 48:1, s. 170-174
-
Tidskriftsartikel (refereegranskat)abstract
- Magnetic stars show several types of light variability which is modulated by the stellar rotation. In chemically peculiar stars, the redistribution of the flux in the surface regions with peculiar chemical composition leads to the light variability with a typical amplitude of the order of hundredths of magnitude. The most efficient processes that cause the flux redistribution are bound-bound (line) transitions of iron and bound-free (ionization) transitions of silicon. This type of light variability typically leads to a complex dependence of the amplitude on the wavelength and shows antiphase light curves in the far ultraviolet and visual regions. In hot magnetic stars, the modulation of the stellar wind by the magnetic field and the wind blanketing cause the light variability with a typical amplitude of the order of millimagnitudes. We predict the light variations in selected magnetic hot stars and compare the simulated light curves with light variations derived from observations.
|
|
| 5. |
- Oksala, M. E., et al.
(författare)
-
Mixed poloidal-toroidal magnetic configuration and surface abundance distributions of the Bp star 36 Lyn
- 2018
-
Ingår i: Monthly notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 473:3, s. 3367-3376
-
Tidskriftsartikel (refereegranskat)abstract
- Previous studies of the chemically peculiar Bp star 36 Lyn revealed a moderately strong magnetic field, circumstellar material and inhomogeneous surface abundance distributions of certain elements. We present in this paper an analysis of 33 high signal-to-noise ratio, high-resolution Stokes IV observations of 36 Lyn obtained with the Narval spectropolarimeter at the Bernard Lyot Telescope at Pic du Midi Observatory. From these data, we compute new measurements of the mean longitudinal magnetic field, Bℓ, using the multiline least-squares deconvolution (LSD) technique. A rotationally phased Bℓ curve reveals a strong magnetic field, with indications for deviation from a pure dipole field. We derive magnetic maps and chemical abundance distributions from the LSD profiles, produced using the Zeeman–Doppler imaging code InversLSD. Using a spherical harmonic expansion to characterize the magnetic field, we find that the harmonic energy is concentrated predominantly in the dipole mode (ℓ = 1), with significant contribution from both the poloidal and toroidal components. This toroidal field component is predicted theoretically, but not typically observed for Ap/Bp stars. Chemical abundance maps reveal a helium enhancement in a distinct region where the radial magnetic field is strong. Silicon enhancements are located in two regions, also where the radial field is stronger. Titanium and iron enhancements are slightly offset from the helium enhancements, and are located in areas where the radial field is weak, close to the magnetic equator.
|
|
| 6. |
- Silvester, James
(författare)
-
Modelling complex magnetic fields in stars with radiative envelopes
- 2018
-
Ingår i: CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO. - : SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST. - 1335-1842. ; 48:1, s. 116-123
-
Tidskriftsartikel (refereegranskat)abstract
- Magnetic chemically peculiar A and B type stars (Ap/Bp) exhibit strong globally organised magnetic fields, this is combined with strong chemical abundance non-uniformities within the atmosphere. The presence of the magnetic field influences energy and mass transport within the atmosphere of a star, this is thought to cause these observed chemical non-uniformities. These stars offer the ideal laboratory for understanding the interplay between magnetic field structure, atmospheric transport processes and other stellar parameters. With the recent increase in the availability of spectropolarimetric data and by using magnetic Doppler imaging (MDI) techniques, the number of detailed maps of the magnetic structure of Ap/Bp stars is growing. It is now possible to begin to investigate correlations between the magnetic field structure, chemical abundance structures in the photospheres of Ap/Bp stars and other stellar parameters, the first steps in understanding the evolution of such magnetic fields.
|
|
| 7. |
- Silvester, James, et al.
(författare)
-
The magnetic field topology and chemical abundance distributions of the Ap star HD 32633
- 2015
-
Ingår i: Monthly notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 453:2, s. 2163-2176
-
Tidskriftsartikel (refereegranskat)abstract
- Previous observations of the Ap star HD 32633 indicated that its magnetic field was unusually complex in nature and could not be characterized by a simple dipolar structure. Here we derive magnetic field maps and chemical abundance distributions for this star using full Stokes vector (Stokes IQUV) high-resolution observations obtained with the ESPaDOnS and Narval spectropolarimeters. Our maps, produced using the INVERS 10 magnetic Doppler imaging (MDI) code, show that HD 32633 has a strong magnetic field which features two large regions of opposite polarity but deviates significantly from a pure dipole field. We use a spherical harmonic expansion to characterize the magnetic field and find that the harmonic energy is predominately in the l = 1 and 2 poloidal modes with a small toroidal component. At the same time, we demonstrate that the observed Stokes parameter profiles of HD 32633 cannot be fully described by either a dipolar or dipolar plus quadrupolar field geometry. We compare the magnetic field topology of HD 32633 with other early-type stars for which MDI analyses have been performed, supporting a trend of increasing field complexity with stellar mass. We then compare the magnetic field topology of HD 32633 with derived chemical abundance maps for the elements Mg, Si, Ti, Cr, Fe, Ni and Nd. We find that the iron-peak elements show similar distributions, but we are unable to find a clear correlation between the location of local chemical enhancements or depletions and the magnetic field structure.
|
|
| 8. |
- Wade, G. A., et al.
(författare)
-
Magnetic B stars observed with BRITE : Spots, magnetospheres, binarity, and pulsations
- 2017
-
Ingår i: Second brite-constellation science conference. - Warsaw : POLISH ASTRONOMICAL SOC. - 9788393827961 ; , s. 94-100
-
Konferensbidrag (refereegranskat)abstract
- Magnetic B-type stars exhibit photometric variability due to diverse causes, and consequently on a variety of timescales. In this paper we describe interpretation of BRITE photometry and related ground-based observations of four magnetic B-type systems: epsilon Lupi, tau Sco, a Cen and epsilon CMa.
|
|
