intrinsic colour
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2022 ◽  
Vol ahead-of-print (ahead-of-print) ◽  
Author(s):  
Raffaele Zanchini ◽  
Simone Blanc ◽  
Liam Pippinato ◽  
Giuseppe Di Vita ◽  
Filippo Brun

PurposeAs is well known, there are several aspects that characterise honey consumption and the reasons for purchasing it. Despite this, little attention has been paid to the drivers that move consumers towards the use of honey for its health benefits and therapeutic properties. The aim of this study is to define which drivers move the consumption of honey for its health benefits.Design/methodology/approachThe study, conducted on 640 Italian honey consumers, applied inferential tests (Chi-square) and an econometric model (logit regression), and showed that about 66% of the respondents stated that they consume honey for its health properties.FindingsThe main drivers of honey consumption are both among the intrinsic (Colour) and extrinsic (Origin and Organic certification) attributes of the product. What also emerges is that the propensity to consume honey for health purposes is influenced by the consumer characteristics and habits, such as Age cohort, Gender, BMI and Large retail buyer. Moreover, we observed that consumption is influenced by BMI but not by lifestyle characteristics such as sport and diet.Originality/valueThis study could be a support tool for policymakers who are interested in promoting good nutrition and improving public health, since there is great interest in the functional properties of foods and the need to enhance the value of products, while at the same time ensuring consumer protection.


2020 ◽  
Vol 496 (3) ◽  
pp. 3887-3905 ◽  
Author(s):  
Z Eker ◽  
F Soydugan ◽  
S Bilir ◽  
V Bakış ◽  
F Aliçavuş ◽  
...  

ABSTRACT Nearby detached double-lined eclipsing binaries with most accurate data were studied and 290 systems were found with at least one main-sequence component having a metallicity of 0.008 ≤ Z ≤ 0.040. Stellar parameters, light ratios, Gaia Data Release 2 trigonometric parallaxes, extinctions and/or reddening were investigated and only 206 systems were selected as eligible to calculate empirical bolometric corrections. NASA/IPAC Galactic dust maps were the main source of extinctions. Unreliable extinctions at low Galactic latitudes |b| ≤ 5° were replaced with individual determinations, if they exist in the literature, else associated systems were discarded. The main-sequence stars of te remaining systems were used to calculate the bolometric corrections (BCs) and to calibrate the BC–Teff relation, which is valid in the range 3100–36 000 K. De-reddened (B − V)0 colours, on the other hand, allowed us to calibrate two intrinsic colour–effective temperature relations; the linear one is valid for $T_{\rm eff}\gt 10\, 000$ K, while the quadratic relation is valid for $T_{\rm eff}\lt 10\, 000$ K; that is, both are valid in the same temperature range in which the BC–Teff relation is valid. New BCs computed from Teff and other astrophysical parameters are tabulated, as well.


Author(s):  
Anne-Isabelle Bidegaray ◽  
Karin Nys ◽  
Alberta Silvestri ◽  
Peter Cosyns ◽  
Wendy Meulebroeck ◽  
...  

2012 ◽  
Vol 8 (S289) ◽  
pp. 195-202
Author(s):  
Alexey S. Rastorguev ◽  
Andrey K. Dambis ◽  
Marina V. Zabolotskikh ◽  
Leonid N. Berdnikov ◽  
Natalia A. Gorynya

AbstractThe Baade–Becker–Wesselink (BBW) method remains one of most often used tools to derive a full set of Cepheid astrophysical parameters. The surface brightness version of the BBW technique was preferentially used during the past few decades to calculate Cepheid radii and to improve period–luminosity–colour relations. Its implementation requires a priori knowledge of Cepheid reddening values. We propose a new version of the BBW technique, which allows one to independently determine the colour excess and the intrinsic colour of a radially pulsating star, in addition to its radius, luminosity and distance. The new technique is a generalization of the Balona light curve-modelling approach. The method also allows calibration of the function F(CI0) = BC(CI0) + 10 log [Teff (CI0)] for the class of pulsating stars considered. We apply this technique to a number of classical Cepheids with very accurate light and radial-velocity curves. The new technique can also be applied to other pulsating variables, e.g., RR Lyrae stars. We also discuss the possible dependence of the projection factor on the pulsation phase.


2011 ◽  
Vol 11 (11) ◽  
pp. 400-400
Author(s):  
R. Fleming ◽  
M. Wolff

New Astronomy ◽  
2010 ◽  
Vol 15 (5) ◽  
pp. 444-449 ◽  
Author(s):  
Yüksel Karataş ◽  
William J. Schuster
Keyword(s):  

2009 ◽  
Vol 396 (3) ◽  
pp. 1573-1578 ◽  
Author(s):  
Ignacio Ferreras ◽  
Thorsten Lisker ◽  
Anna Pasquali ◽  
Sadegh Khochfar ◽  
Sugata Kaviraj

2003 ◽  
Vol 404 (3) ◽  
pp. 901-912 ◽  
Author(s):  
S. Nobili ◽  
A. Goobar ◽  
R. Knop ◽  
P. Nugent

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