The solar chemical composition

Asplund, Martin; Grevesse, N.; Sauval, A. J.

doi:10.1016/j.nuclphysa.2005.06.010

Cited by 277 publications

(352 citation statements)

References 57 publications

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“…This value is well within uncertainty of the solar value Z ⊙ = 0.0122 reported by Asplund et al (2005). …”

Section: Atmospheric Parameters and Abundance Analysissupporting

confidence: 89%

“…The Na abundance was derived from the Na doublet at 5682 & 5688 Å which is subject to non-LTE effects, and therefore is clearly overestimated. Excluding these two odd ions, DD UMa has solar abundances with a metallicity Abundance Relative to the Sun ELODIE HIDES Figure 2: The difference between our derived abundances and the solar abundances of Asplund et al (2005) for ELODIE (filled square) and HIDES (empty circle) spectra of DD UMa. The abundance error bars of ELODIE and HIDES spectra are 0.28 and 0.33 dex respectively, reflecting the systematic uncertainty due to atmospheric parameters.…”

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 97%

“…We adopted the Asplund et al (2005) solar abundances as the initial point from which to begin the fitting process. Table 2 presents the average abundance values and estimated internal error of each ion, for both the ELODIE and HIDES observations.…”

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 99%

“…where a is the atomic number of an element with atomic mass m a and solar abundances from Asplund et al (2005) were adopted for all the elements that we did not analyse. This value is well within uncertainty of the solar value Z ⊙ = 0.0122 reported by Asplund et al (2005).…”

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 99%

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A spectroscopic study of DD UMa: Ursa Major group member and candidate for BRITE

Elmaslı¹,

Fossati²,

Folsom³

et al. 2012

New Astronomy

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The Ursa Major group is a nearby stellar supercluster which, while not gravitationally bound, is defined by co-moving members. DD UMa is a δ Scuti star whose membership in the Ursa Major group is unclear.The objective of this study is to confirm the membership of DD UMa in the Ursa Major group, as well as perform a detailed spectral analysis of the star. Since DD UMa is a low-amplitude δ Scuti star, we performed a frequency analysis. We determined fundamental parameters, chemical abundances, and derive a mass and age for the star.For this study we observed DD UMa at the Okayama Astrophysical Observatory with the high-resolution spectrograph HIDES, between the 27 th of February and the 4 th March, 2009. Additional observations were extracted from the ELODIE archive in order to expand our abundance analysis. Group membership of DD UMa was assessed by examining the velocity of the star in Galactic coordinates. Pulsational frequencies were determined by examining line profile variability in the HIDES spectra. Stellar fundamental parameters and chemical abundances were derived by fitting synthetic spectra to both the HIDES and ELODIE observations. DD UMa is found to be a member of the extended stream of the Ursa Major group, based on the space motion of the star. This is supported by the chemical abundances of the star being consistent with those of Ursa Major group members. The star is found to be chemically solar, with T e f f = 7450 ± 150 K and log g = 3.98 ± 0.2. We found pulsational frequencies of 9.4 c/d and 15.0 c/d. While these frequencies are insufficient to perform an asteroseismic study, DD UMa is a good bright star candidate for future study by the BRITE-constellation.

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“…This value is well within uncertainty of the solar value Z ⊙ = 0.0122 reported by Asplund et al (2005). …”

Section: Atmospheric Parameters and Abundance Analysissupporting

confidence: 89%

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 97%

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 99%

Section: Atmospheric Parameters and Abundance Analysismentioning

confidence: 99%

See 2 more Smart Citations

A spectroscopic study of DD UMa: Ursa Major group member and candidate for BRITE

Elmaslı¹,

Fossati²,

Folsom³

et al. 2012

New Astronomy

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“…The chemical network equations is solved by the CVODE package (Hindmarsh et al 2005). We assume that a gas has solar metallicity with the abundances given in Asplund et al (2005) We suppose that silicon is singly ionized and oxygen stays neutral.…”

Section: Modelmentioning

confidence: 99%

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

Khoperskov

Vasiliev

2017

Monthly Notices of the Royal Astronomical Society

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Using N -body/gasdynamic simulations of a Milky Way-like galaxy we analyse a Kennicutt-Schmidt relation, Σ SFR ∝ Σ gas N , at different spatial scales. We simulate synthetic observations in CO lines and UV band. We adopt the star formation rate (SFR) defined in two ways: based on free fall collapse of a molecular cloud -Σ SFR, cl , and calculated by using a UV flux calibration -Σ SFR, UV . We study a KS relation for spatially smoothed maps with effective spatial resolution from molecular cloud scales to several hundred parsecs. We find that for spatially and kinematically resolved molecular clouds the Σ SFR, cl ∝ Σ gas N relation follows the power-law with index N ≈ 1.4. Using UV flux as SFR calibrator we confirm a systematic offset between the Σ SFR, UV and Σ gas distributions on scales compared to molecular cloud sizes. Degrading resolution of our simulated maps for surface densities of gas and star formation rates we establish that there is no relation Σ SFR, UV − Σ gas below the resolution ∼ 50 pc. We find a transition range around scales ∼ 50 − 120 pc, where the power-law index N increases from 0 to 1 − 1.8 and saturates for scales larger ∼ 120 pc. A value of the index saturated depends on a surface gas density threshold and it becomes steeper for higher Σ gas threshold. Averaging over scales with size of > ∼ 150 pc the power-law index N equals 1.3 − 1.4 for surface gas density threshold ∼ 5 M ⊙ pc −2 . At scales > ∼ 120 pc surface SFR densities determined by using CO data and UV flux, Σ SFR, UV /Σ SFR, cl , demonstrate a discrepancy about a factor of 3. We argue that this may be originated from overestimating (constant) values of conversion factor, star formation efficiency or UV calibration used in our analysis.

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Extinct Radionuclides and the Earliest Differentiation of the Earth and Moon

Caro¹,

Kleine

2010

Timescales of Magmatic Processes

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The solar chemical composition

Cited by 277 publications

References 57 publications

A spectroscopic study of DD UMa: Ursa Major group member and candidate for BRITE

A spectroscopic study of DD UMa: Ursa Major group member and candidate for BRITE

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

Extinct Radionuclides and the Earliest Differentiation of the Earth and Moon

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