- ID:
- ivo://CDS.VizieR/J/A+A/416/655
- Title:
- Atomic lines in IR spectra for ultracool dwarfs
- Short Name:
- J/A+A/416/655
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We provide a set of atomic lines which are suitable for the description of ultracool dwarf spectra from 10000 to 25000{AA}. This atomic linelist was made using both synthetic spectra calculations and existing atlases of infrared spectra of Arcturus and Sunspot umbra. We present plots which show the comparison of synthetic spectra and observed Arcturus and Sunspot umbral spectra for all atomic lines likely to be observable in high resolution infrared spectra.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/157/153
- Title:
- Atomic lines in spectra of RR Lyrae & RHB stars
- Short Name:
- J/AJ/157/153
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have derived relations between FWHMs and equivalent widths of metallic absorption lines in the spectra of RR Lyrae stars to estimate new upper limits on the axial equatorial rotational velocities of RR Lyrae and metal-poor red horizontal branch (RHB) stars. We have also derived the variations of RR Lyrae macroturbulent velocities during the pulsation cycles. In RRab cycles, the line widths are dominated by phase-dependent convolutions of axial rotation and macroturbulence, which we designate as V_macrot_. The behavior of V_macrot_ is remarkably uniform among the RRab stars, but the behavior of V_macrot_ among RRc stars varies strongly from star to star. The RRab stars exhibit an upper limit on V_macrot_ of 5+/-1 km/s with weak evidence of an anticorrelation with T_eff_. The RRc minima range from 2 to 12 km/s. The abrupt decline in large rotations with decreasing T_eff_ at the blue boundary of the instability strip and the apparently smooth continuous variation among the RRab and RHB stars suggests that HB stars gain/lose surface angular momentum on timescales that are short compared to HB lifetimes. The V_macrot_ values for our metal-poor RHB stars agree well with those derived by Fourier analysis of an independent but less metal-poor sample of Carney et al. (2008AJ....135..892C); they conform qualitatively to the expectations of Tanner et al. (2013ApJ...778..117T). A general conclusion of our investigation is that surface angular momentum as measured by V_rot_sin(i) is not a reliable indicator of total stellar angular momentum anywhere along the HB.
1533. Atomic mass excesses
- ID:
- ivo://CDS.VizieR/J/ApJ/844/139
- Title:
- Atomic mass excesses
- Short Name:
- J/ApJ/844/139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- X-ray burst model predictions of light curves and the final composition of the nuclear ashes are affected by uncertain nuclear masses. However, not all of these masses are determined experimentally with sufficient accuracy. Here we identify the remaining nuclear mass uncertainties in X-ray burst models using a one-zone model that takes into account the changes in temperature and density evolution caused by changes in the nuclear physics. Two types of bursts are investigated-a typical mixed H/He burst with a limited rapid proton capture process (rp-process) and an extreme mixed H/He burst with an extended rp-process. When allowing for a 3{sigma} variation, only three remaining nuclear mass uncertainties affect the light-curve predictions of a typical H/He burst (^27^P, ^61^Ga, and ^65^As), and only three additional masses affect the composition strongly (^80^Zr, ^81^Zr, and ^82^Nb). A larger number of mass uncertainties remain to be addressed for the extreme H/He burst, with the most important being ^58^Zn, ^61^Ga, ^62^Ge, ^65^As, ^66^Se, ^78^Y, ^79^Y, ^79^Zr, ^80^Zr, ^81^Zr, ^82^Zr, ^82^Nb, ^83^Nb, ^86^Tc, ^91^Rh, ^95^Ag, ^98^Cd, ^99^In, ^100^In, and ^101^In. The smallest mass uncertainty that still impacts composition significantly when varied by 3{sigma} is ^85^Mo with 16keV uncertainty. For one of the identified masses, ^27^P, we use the isobaric mass multiplet equation to improve the mass uncertainty, obtaining an atomic mass excess of -716(7)keV. The results provide a roadmap for future experiments at advanced rare isotope beam facilities, where all the identified nuclides are expected to be within reach for precision mass measurements.
- ID:
- ivo://CDS.VizieR/VI/69
- Title:
- Atomic Spectral Line List
- Short Name:
- VI/69
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This compilation is aimed at providing a general catalog of atomic lines for comparatively low-ionized species, laying emphasis on their transition probabilities. Please refer to file "explain" for a detailed description.
- ID:
- ivo://CDS.VizieR/VI/73
- Title:
- Atomic Spectral Lines Data OII, Mg, Al, S, Sc
- Short Name:
- VI/73
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Atomic Spectral Lines Data O II, Mg I-XII, Al I-XIII, S I-XVI, Sc I-XXI. Using recent critical compilations of atomic energy levels, the authors calculate wavelengths (or wave numbers) from the differences of the energy levels. Results are given along with the observed values for all classified lines. Unless otherwise noted, the calculated values are in general more accurate than the observed values wherever the two values differ significantly. Some observed lines are classified as unresolved blends of two or more transitions. The calculated wavelength for each of the main components of such a blend is listed, or in some cases the calculated wavelength of the probable strongest component.
- ID:
- ivo://CDS.VizieR/J/ApJS/194/35
- Title:
- Atomic transition probabilities of Mn
- Short Name:
- J/ApJS/194/35
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The goal of the present work is to produce transition probabilities with very low uncertainties for a selected set of multiplets of MnI and MnII. Multiplets are chosen based upon their suitability for stellar abundance analysis. We report on new radiative lifetime measurements for 22 levels of MnI from the e^8^D, z^6^P, z^6^D, z^4^F, e^8^S, and e^6^S terms and six levels of MnII from the z^5^P and z^7^P terms using time-resolved laser-induced fluorescence on a slow atom/ion beam. New branching fractions for transitions from these levels, measured using a Fourier-transform spectrometer, are reported.
- ID:
- ivo://CDS.VizieR/VI/72
- Title:
- Atomic Transition Probabilities, Sc-Ni
- Short Name:
- VI/72
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Atomic transition probabilities for Scandium (Z = 21) through Ni (Z = 28) for about 18,300 spectral lines are critically compiled, based on all available literature sources. The transition probability data, oscillator strengths, and line shape data were collected, catalogued and evaluated by the Data Center on Atomic Transition Probabilities at the National Institute of Standards and Technology, USA (NIST).
- ID:
- ivo://CDS.VizieR/J/A+A/584/A72
- Title:
- A transiting rocky planet at 6.5pc from the Sun
- Short Name:
- J/A+A/584/A72
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V=5.5) and close-by (6.5pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935+/-0.0003-days, on a quasi-circular orbit with a semi-major axis of 0.0382+/-0.0003AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date.
- ID:
- ivo://cdpp/transplanet/q/epn_core
- Title:
- A Transplanet model of magnetosphere-ionosphere coupling at Earth, Mars and Jupiter
- Short Name:
- transplanet.epn_
- Date:
- 11 Jul 2024 07:32:35
- Publisher:
- CDPP - Centre de Données de la Physique des Plasmas
- Description:
- Transplanet runs
- ID:
- ivo://CDS.VizieR/J/ApJS/99/135
- Title:
- A-type stars rotation and spectral peculiarities
- Short Name:
- J/ApJS/99/135
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We obtained new data to determine whether the spectral appearance of A-type stars is entirely determined by their rotational velocities. For this purpose we derived rotational velocities for 1700 northern A-type stars from CCD coude spectra, calibrated with the new Slettebak et al. system, and new MK classifications based on wide photographic Cassegrain spectra for 2000 northern and some southern stars in the Bright Star Catalogue. In addition we determined the equivalent widths of the lambda 4481 Mg II lines in the coude spectra. Tables and graphs show variations of rotational velocities and lambda 4481 line strengths as functions of type and luminosity, and frequencies of the normal and abnormal stars. After deconvolutions of the rotational velocities, assuming random orientations of rotational axes, we find that all rapid rotators have normal spectra and nearly all slow rotators have abnormal spectra (Ap or Am). Those abnormalities are generally attributed to diffusion and can occur only with little rotational mixing. However at all types there are overlaps of these distributions, implying that a given intermediate rotational velocity is insufficient to determine whether the star should have a normal or abnormal spectrum. However, we realized that (1) some of our "standards," such as Vega and Alpha Dra, are really abnormal, causing us to classify similar peculiar stars as "normal," (2) many of the "normal" stars near A2 IV have the characteristics of peculiar stars such as low rotational velocities and weak 4481 Mg II and K lines, and (3) the mean rotational velocities of "normal" stars are depressed just at those types where the Ap and Am stars are most frequent. Therefore we conclude that the overlaps are due to our failure to detect all the abnormal stars and that a specific rotational velocity is probably enough to determine whether a star will have a normal or abnormal spectrum.
