U, b, v, Observations of U SGR.

Mitchell, R. I.; Johnson, Harold L.; Iriarte, B.

doi:10.1086/147114

Cited by 6 publications

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“…Photometric investigations of the variable include Abt and Hardie (1960), Preston and Kilston (1967), Oosterhoff (1957), Mitchell et al (1964), Michalowska and Smak (1965), Moffett and Barnes (1984), and Smith et al (1978).…”

Section: Introductionmentioning

confidence: 99%

A photometric study of BL Herculis

Alexander¹,

Joner²,

McNamara³

1987

PASP

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Photometric (■ uvby ß) observations of the prototype variable BL Her are described. The photometry indicates the variable is reddened. We have adoptedE(b-y) = 07055. Intrinsic (b-y) and c 1 values are used to derive the mean temperature and surface gravity (T eff ) = 6660 K, and (log g) = 2.46. The (rrq) 0 index at light minimum is (rrq) 0 = 0.198, indicating the variable is very metal strong. We infer that [Fe/H] = +0.20. An application of a modified Baade-Wesselink analysis to the photometric and radial-velocity data in the phase interval 0.45 < c|> < 0.775, when most of the light variation can be attributed to a change in radius, yields (R) = 8.5 R ö and (M v ) = -0.5. The radius and surface gravity indicate that the mass is 3Jt -0.75 3W 0 .

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Section: Introductionmentioning

confidence: 99%

A photometric study of BL Herculis

Alexander¹,

Joner²,

McNamara³

1987

PASP

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“…Irwin's data were communicated to Johnson in 1957, and70 stars in common with Johnson (1960) were used to transform Irwin's instrumental system to Johnson's M 25 magnitude scale. Sandage's (1960) data were corrected as indicated by Mitchell, Johnson, and Iriarte (1961). The data by Wampler, Pesch, Hiltner, and Kraft (1961) were corrected to Johnson's system on the basis of data presented by Landolt (1964)…”

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confidence: 99%

A New Variable in M 25

Mitchell¹

1967

PASP

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Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

Marco

Bernabeu

Negueruela

2001

The Astronomical Journal

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We present uvbyb CCD photometry of the Ðeld of the open cluster NGC 1893. Our photometry is deep enough to cover the complete main-sequence B spectral type. We identify D50 very likely members of the cluster down to spectral type B9ÈA0, some of which have much higher reddenings than the average. We derive a color excess E(b[y) \ 0.33^0.03 and a dereddened distance modulus V 0 [M V \ 13.9^0.2. From the b index, we identify several candidates as emission-line stars, for which we have obtained spectroscopy. Three of them display spectra corresponding to spectral type F but showing Ha in emission. Photometric measurements in this and previous studies indicate strong variability. These characteristics show them to be preÈmain-sequence stars of spectral type F. We also identify two likely Herbig Be stars. These results hint at the existence of a sizable preÈmain-sequence population in NGC 1893.

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U, b, v, Observations of U SGR.

Cited by 6 publications

References 0 publications

A photometric study of BL Herculis

A photometric study of BL Herculis

A New Variable in M 25

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

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