5.3.1.3.1 Empirical determination of the wavelength-dependence of the absorption coefficient for the sun

Author(s):  
E. Böhm-Vitense

2021 ◽  
Author(s):  
Jesús Yus-Díez ◽  
Vera Bernardoni ◽  
Griša Močnik ◽  
Andrés Alastuey ◽  
Davide Ciniglia ◽  
...  

Abstract. Accurate measurements of light absorption by aerosolized particles, especially black carbon (BC), are of utter importance since BC represents the second most important climate-warming agent after carbon dioxide (CO2). Reducing the uncertainties related to the absorption measurement techniques will improve the global estimation of BC concentration and the radiative effects of light absorbing aerosols. Currently, one of the most widely used instruments for BC and absorption measurements is the dual-spot aethalometer, AE33, which derives the absorption coefficients of aerosol particles at 7 different wavelengths from the measurements of optical attenuation through a filter where particles are continuously collected. An accurate determination of the absorption coefficient relies on the quantification of non-linear processes related to the collection of sample on the filter. The multiple-scattering correction factor (C(λ)), which depends on the filter tape used and on the optical properties of the collected particles, is the parameter with the greatest uncertainty.An in-depth analysis of the AE33 multiple-scattering correction factor and its wavelength dependence for different filter tapes, i.e. the old most referenced known as TFE-coated glass and the current most widely used M8060, has been carried out by comparing the AE33 attenuation measurements with the absorption measurements from different filter-based techniques. Online co-located multi-angle absorption photometer (MAAP) measurements and offline PP_UniMI polar photometer measurements were used with this aim. We used data from three different measurement stations in North-East of Spain: an urban background station (Barcelona; BCN), a regional background station (Montseny; MSY) and a mountain-top station (Montsec d'Ares; MSA). The median C values (at 637 nm) measured at the three stations ranged between 2.29 (at BCN and MSY; lowest 5th percentile of 1.97 and highest 95th percentile of 2.68) and 2.51 (at MSA; lowest 5th percentile of 2.06 and highest 95th percentile of 3.06). The C factor was wavelength-dependent only at the mountain-top station, whereas at the urban and regional stations no statistically significant difference was found at the 7 different AE33 wavelengths. The wavelength-dependence of C at the mountain station was in part driven by the predominant effect of dust particles during Saharan dust outbreaks at this station. At the mountain station, neglecting the wavelength dependence of the C factor led to an underestimation of the Absorption Ångström Exponent (AAE) of 12 %. The analysis of the cross-sensitivity to scattering for different filter tapes revealed a large increase of the C factor at the three stations when the single scattering albedo (SSA) of the collected particles was above 0.90–0.95, with up to a 3-fold increase above the average values. The result of the cross-sensitivity to scattering displayed a fitted constant multiple scattering parameter, Cf, of 2.21 and 1.96 and a cross-sensitivity factor, ms, of 0.8 % and 1.7 % for MSY and MSA stations, respectively, for the TFE-coated glass filter tape. For the M8060 filter tape, Cf of 2.50, 1.96, 1.82 and a ms of 0.7 %, 1.5 %, 2.7 %, for BCN, MSY and MSA stations, respectively, were obtained. Differences in the absorption coefficient determined from AE33 measurements at BCN, MSY and MSA of around a 35–40 % can be expected when using the site-dependent C determined experimentally instead of the nominal C value.



2016 ◽  
Vol 459 (2) ◽  
pp. 1646-1658 ◽  
Author(s):  
Christopher J. R. Clark ◽  
Simon P. Schofield ◽  
Haley L. Gomez ◽  
Jonathan I. Davies


1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.



2017 ◽  
Vol 12 (S330) ◽  
pp. 148-151 ◽  
Author(s):  
Edouard J. Bernard

AbstractWe took advantage of the Gaia DR1 to combine TGAS parallaxes with Tycho-2 and APASS photometry to calculate the star formation history (SFH) of the solar neighbourhood within 250 pc using the colour-magnitude diagram fitting technique. We present the determination of the completeness within this volume, and compare the resulting SFH with that calculated from the Hipparcos catalogue within 80 pc of the Sun. We also show how this technique will be applied out to ~5 kpc thanks to the next Gaia data releases, which will allow us to quantify the SFH of the thin disc, thick disc and halo in situ, rather than extrapolating based on the stars from these components that are today in the solar neighbourhood.



2021 ◽  
Vol 18 (1) ◽  
Author(s):  
Jørgen Christensen-Dalsgaard

AbstractThe Sun provides a critical benchmark for the general study of stellar structure and evolution. Also, knowledge about the internal properties of the Sun is important for the understanding of solar atmospheric phenomena, including the solar magnetic cycle. Here I provide a brief overview of the theory of stellar structure and evolution, including the physical processes and parameters that are involved. This is followed by a discussion of solar evolution, extending from the birth to the latest stages. As a background for the interpretation of observations related to the solar interior I provide a rather extensive analysis of the sensitivity of solar models to the assumptions underlying their calculation. I then discuss the detailed information about the solar interior that has become available through helioseismic investigations and the detection of solar neutrinos, with further constraints provided by the observed abundances of the lightest elements. Revisions in the determination of the solar surface abundances have led to increased discrepancies, discussed in some detail, between the observational inferences and solar models. I finally briefly address the relation of the Sun to other similar stars and the prospects for asteroseismic investigations of stellar structure and evolution.



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