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   <subfield code="D">V.</subfield>
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   <subfield code="a">Estimation of the solar galactocentric distance and galactic rotation velocity from near-solar-circle objects</subfield>
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   <subfield code="c">[V. Bobylev]</subfield>
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   <subfield code="a">We have tested the method of determining the solar Galactocentric distance R 0 and Galactic rotation velocity V 0 modified by Sofue et al. using near-solar-circle objects. The motion of objects relative to the local standard of rest has been properly taken into account. We show that when such young objects as star-forming regions or Cepheids are analyzed, allowance for the perturbations produced by the Galactic spiral density wave improves the statistical significance of the estimates. The estimate of R 0 = 7.25 ± 0.32 kpc has been obtained from 19 star-forming regions. The following estimates have been obtained from a sample of 14 Cepheids (with pulsation periods P &gt; 5 d ): R 0 = 7.66 ± 0.36 kpc and V 0 = 267 ± 17 km s−1. We consider the influence of the adopted Oort constant A and the character of stellar proper motions (Hipparcos or UCAC4). The following estimates have been obtained from a sample of 18 Cepheids with stellar proper motions from the UCAC4 catalog: R 0 = 7.64 ± 0.32 kpc and V 0 = 217 ± 11 km s−1.</subfield>
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   <subfield code="a">star-forming regions</subfield>
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   <subfield code="a">solar Galactocentric distance</subfield>
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   <subfield code="a">Galactic rotation velocity</subfield>
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   <subfield code="t">Astronomy Letters</subfield>
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   <subfield code="g">39/2(2013-02-01), 95-103</subfield>
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   <subfield code="a">Metadata rights reserved</subfield>
   <subfield code="b">Springer special CC-BY-NC licence</subfield>
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