Talk:30 Arietis: Difference between revisions

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Revision as of 15:26, 3 May 2014 edit77.57.25.250 (talk) →30 Ari A: Guenther et al. (2009) demonstrates that 30 Ari A is still on the main sequence← Previous edit		Revision as of 21:26, 4 March 2015 edit undoArtman40 (talk \| contribs)2,039 editsNo edit summaryNext edit →
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	:<blockquote>30 Ari A is listed in the SIMBAD database with a spectral type F6III. If true, the object should have an absolute brightness (<var>M<sub>v</sub></var>) of +1.4 mag. Using again the Hipparcos distance, the relative magnitude (<var>m<sub>v</sub></var>) would than be 4.4 mag, which is inconsistent with the observed brightness (Table 1). The <var>V</var> − <var>J</var> colours are 0.808 ± 0.02 for 30 Ari A and 1.02 ± 0.02 for 30 Ari B, and the <var>V</var> − <var>K</var> colours are 1.01±0.3 and 1.27±0.02 for components A and B, respectively. The colours are also inconsistent with a giant star but consistent with a main-sequence star. Using our high resolution spectra (see Sect. 3) and following the method described in Frasca et al. (2003) and Gandolfi et al. (2008), we find that 30 Ari A is an F5V star and 30 Ari B, and 30 Ari B and F6V star (Figs. 1; 2). Thus, the brightness, colours and the results of the spectroscopy show that both components are still on the main sequence stars.</blockquote>		:<blockquote>30 Ari A is listed in the SIMBAD database with a spectral type F6III. If true, the object should have an absolute brightness (<var>M<sub>v</sub></var>) of +1.4 mag. Using again the Hipparcos distance, the relative magnitude (<var>m<sub>v</sub></var>) would than be 4.4 mag, which is inconsistent with the observed brightness (Table 1). The <var>V</var> − <var>J</var> colours are 0.808 ± 0.02 for 30 Ari A and 1.02 ± 0.02 for 30 Ari B, and the <var>V</var> − <var>K</var> colours are 1.01±0.3 and 1.27±0.02 for components A and B, respectively. The colours are also inconsistent with a giant star but consistent with a main-sequence star. Using our high resolution spectra (see Sect. 3) and following the method described in Frasca et al. (2003) and Gandolfi et al. (2008), we find that 30 Ari A is an F5V star and 30 Ari B, and 30 Ari B and F6V star (Figs. 1; 2). Thus, the brightness, colours and the results of the spectroscopy show that both components are still on the main sequence stars.</blockquote>
	:] (]) 15:26, 3 May 2014 (UTC)		:] (]) 15:26, 3 May 2014 (UTC)

			==Quadruple star==

			Apparently, some new vital information about the star system came available. http://www.nasa.gov/jpl/planet-reared-by-four-parent-stars/index.html#.VPd3LM2glZ4 --] (]) 21:26, 4 March 2015 (UTC)

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30 Ari A

An unsourced sentence in the text describes both as F-type main-sequence stars based on luminosity, yet SIMBAD lists the A component as a giant. Further, the luminosity listed for the A component in the Details section of the starbox (1.991 solar) is consistent with neither the absolute magnitude (abs mag of 3.46 suggests a luminosity well in excess of 3 solar) nor the difference in magnitude between the two stars (7.09 - 6.48 = 0.61, which indicates 30 Ari A should be at least 75% brighter than 30 Ari B, rather than nearly the same). Given these discrepancies, I've updated the starbox with the data from SIMBAD and altered the luminosity of the A component. Pfhreak (talk) 15:38, 27 January 2013 (UTC)

See the paper Guenther et al. (2009) "A substellar component orbiting the F-star 30 Arietis B" (referenced in the article) for more about this:

30 Ari A is listed in the SIMBAD database with a spectral type F6III. If true, the object should have an absolute brightness (M_v) of +1.4 mag. Using again the Hipparcos distance, the relative magnitude (m_v) would than be 4.4 mag, which is inconsistent with the observed brightness (Table 1). The V − J colours are 0.808 ± 0.02 for 30 Ari A and 1.02 ± 0.02 for 30 Ari B, and the V − K colours are 1.01±0.3 and 1.27±0.02 for components A and B, respectively. The colours are also inconsistent with a giant star but consistent with a main-sequence star. Using our high resolution spectra (see Sect. 3) and following the method described in Frasca et al. (2003) and Gandolfi et al. (2008), we find that 30 Ari A is an F5V star and 30 Ari B, and 30 Ari B and F6V star (Figs. 1; 2). Thus, the brightness, colours and the results of the spectroscopy show that both components are still on the main sequence stars.

77.57.25.250 (talk) 15:26, 3 May 2014 (UTC)

Quadruple star

Apparently, some new vital information about the star system came available. http://www.nasa.gov/jpl/planet-reared-by-four-parent-stars/index.html#.VPd3LM2glZ4 --Artman40 (talk) 21:26, 4 March 2015 (UTC)

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