Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer

Nordgren, Tyler E.; Germain, M. E.; Benson, J. A.; Mozurkewich, David; Sudol, Jeffrey J.; Elias, N. M.; Hajian, Arsen R.; White, N. M.; Hutter, D. J.; Johnston, K. J.; Gauss, F. S.; Armstrong, J. T.; Pauls, T.; Rickard, L. J.

doi:10.1086/301114

Cited by 86 publications

(57 citation statements)

References 14 publications

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“…Our solution, close to the DMSA/O one, gives a radius of 12 R (1.2 mas) for the 2 M giant, in perfect agreement with the value obtained by Nordgren et al (1999). The companion should have a mass between 0.4 and 0.5 M and an eclipse would therefore only show a dip of 2-3 mmag.…”

Section: Individual Casessupporting

confidence: 88%

Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries

Pourbaix

Boffin

2003

A&A

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Abstract. By reanalyzing the Hipparcos Intermediate Astrometric Data of a large sample of spectroscopic binaries containing a giant, we obtain a sample of 29 systems fulfilling a carefully derived set of constraints and hence for which we can derive an accurate orbital solution. Of these, one is a double-lined spectroscopic binary and six were not listed in the DMSA/O section of the catalogue. Using our solutions, we derive the masses of the components in these systems and statistically analyze them. We also briefly discuss each system individually.

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Section: Individual Casessupporting

confidence: 88%

Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries

Pourbaix

Boffin

2003

A&A

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“…Mass Age (2003) 7.95±0.09 Nordgren et al (2001) 7.97±0.11 Nordgren et al (2001) 8.035±0.08 Mozurkewich et al (1991) 9.26±0.15 Shao et al (1988) 7.90±0.31 di Benedetto & Rabbia (1987) (2016) 3.722±0.071 Mozurkewich et al (2003) 3.34±0.07 Nordgren et al (2001) 3.68±0.05 Nordgren et al (2001) 148856 3.472±0.008 3.462±0.035 Mozurkewich et al (2003) 3.53±0.08 Nordgren et al (2001) 3.51±0.05 Nordgren et al (2001) 150997 2.493±0.018 2.624±0.034 Mozurkewich et al (2003) 2.50±0.08 Nordgren et al (2001) 2.64±0.04 Nordgren et al (2001) 2.42±0.07 Nordgren et al (1999) 156283 5.519±0.011 5.275±0.067 Mozurkewich et al (2003) 5.26±0.06 Nordgren et al (2001) 5.27±0.07 Nordgren et al (2001) 5.20±0.03 Nordgren et al (1999) (2016) 2.12±0.02 Ligi et al (2012) 2.041±0.043 Baines et al (2010) 172167 3.280±0.016 2.930±0.007 Monnier et al (2012) 3.08±0.03 * Mourard et al (2009) 3.202±0.005 * Absil et al (2006) 3.329±0.006 Aufdenberg et al (2006) 3.225±0.032 Mozurkewich et al (2003) 3.28±0.01 Ciardi et al (2001) Mozurkewich et al (2003) 3.11±0.04 Nordgren et al (2001) 3.20±0.05 Nordgren et al (2001) 3.08±0.03 Nordgren et al (1999) Note- * No LD diameter was provided, therefore we list the UD diameter here. Figure 4 shows a graphical representation of this table.…”

Section: Targetmentioning

confidence: 99%

Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer

et al. 2017

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We present the fundamental properties of 87 stars based on angular diameter measurements from the Navy Precision Optical Interferometer, 36 of which have not been measured previously using interferometry. Our sample consists of 5 dwarfs, 3 subgiants, 69 giants, 3 bright giants, and 7 supergiants, and span a wide range of spectral classes from B to M. We combined our angular diameters with photometric and distance information from the literature to determine each star's physical radius, effective temperature, bolometric flux, luminosity, mass, and age.

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“…However, if several, equidistant spots are present on the surface, then the observed period would be where n is the number of P rot /n, spots, and when phasing the data to the "" observed ÏÏ period, a more sinusoidal variation can result. Nordgren et al (1999) give a radius of 46^3 based R _ on interferometric measurements made with the Navy Prototype Optical Interferometer. An assumed rotational period of 40 days yields an equatorial rotational velocity of 58 km s~1, which implies a stellar inclination of about 8¡.…”

Section: Surface Structurementioning

confidence: 99%

The Radial Velocity and Spectral Line Bisector Variability of Polaris

Hatzes

Cochran

2000

The Astronomical Journal

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We present precise stellar radial velocity measurements for the Cepheid-type star Polaris taken in 1992È1993. The peak-to-peak amplitude of the pulsations was 1.555^0.056 km s~1 in epoch 1992.4 and 1.517^0.047 km s~1 in epoch 1993.2. These amplitudes are comparable to the one measured by Dinshaw et al. in 1987.75 and Mg I j5528 lines also show variations with the 40 day period, strongly indicating that this period is indeed real. The presence of line bisector variations excludes a low-mass companion object as a cause of the residual radial velocity variations. Two models are considered for the residual radial velocity and bisector span variations : starspots and nonradial pulsations. Although both can reproduce the amplitude and shape of the residual radial velocity variations, the spot models considered were unable to reproduce the overall shape and amplitude of the bisector span variations. The best-Ðt spot model was provided by a single spot with a temperature 500 K cooler than the photosphere with a macroturbulent velocity of zero in the spot. If surface features do exist on Polaris and are responsible for the residual radial variations for this star, then possibly they have a temperature structure and distribution more complicated than the simple models considered here. The best Ðt to all the observed variations was provided by a nonradial m \ 4 mode, although these were not entirely satisfactory having a phase shift of about 0.25 between the observed and predicted bisector variations. Possible explanations for this shift include temperature e †ects, a source function originating in a dynamic stellar atmosphere, or a di †erent pulsation mode than the one that was considered. Although the exact pulsational mode is yet to be identiÐed, we believe that the residual radial velocity variations are due to a long-period pulsation mode. Supporting evidence comes from the fact that three di †erent residual variations with periods near 40 days have now been seen in Polaris and it is unlikely that these variations are due to rotational modulation by surface features on a star that is di †erentially rotating.

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Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer

Cited by 86 publications

References 14 publications

Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries

Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries

Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer

The Radial Velocity and Spectral Line Bisector Variability of Polaris

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