[
    {
        "id": "authors:c9v2z-wt579",
        "collection": "authors",
        "collection_id": "c9v2z-wt579",
        "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-094501216",
        "type": "article",
        "title": "The Interpretation of Photoelectric Colors for Stars of Types B-F",
        "author": [
            {
                "family_name": "Bonsack",
                "given_name": "W. K.",
                "clpid": "Bonsack-W-K"
            },
            {
                "family_name": "Greenstein",
                "given_name": "J. L.",
                "clpid": "Greenstein-J-L"
            },
            {
                "family_name": "Mathis",
                "given_name": "J. S.",
                "clpid": "Mathis-J-S"
            },
            {
                "family_name": "Melbourne",
                "given_name": "W. G.",
                "clpid": "Melbourne-W-G"
            },
            {
                "family_name": "Neugebauer",
                "given_name": "G.",
                "clpid": "Neugebauer-G"
            },
            {
                "family_name": "Newburn",
                "given_name": "R. L.",
                "clpid": "Newburn-R-L"
            },
            {
                "family_name": "Olsen",
                "given_name": "K. H.",
                "clpid": "Olsen-K-H"
            },
            {
                "family_name": "Tifft",
                "given_name": "W. G.",
                "clpid": "Tifft-W-G"
            },
            {
                "family_name": "Wahlquist",
                "given_name": "H. D.",
                "clpid": "Wahlquist-H-D"
            },
            {
                "family_name": "Wallerstein",
                "given_name": "G.",
                "orcid": "0000-0003-3416-8728",
                "clpid": "Wallerstein-G"
            }
        ],
        "abstract": "The accumulation of photoelectric data on the Johnson-Morgan system of B - V and U - B colors makes a preliminary theoretical reconnaissance desirable The colors were predicted for atmospheres of a wide range of effective temperatures and electron pressures. The effects of the Balmer jump on the response in the U band and of the Balmer lines in the B band were included, using averages taken over spectral type and luminosity classes. Table 2 gives the predicted fluxes as compared to a black body, the corrected B - V and U - B colors, and the color temperatures The zero point is based on Code's spectral scans of two stars. The results are most useful for  differential effects over small ranges of 0 and P_e; the general temperature and pressure scale derived colorimetrically seems reasonable. The large effect of lines in certain white dwarfs explains some features of the observed colors.",
        "doi": "10.1086/146289",
        "issn": "0004-637X",
        "publisher": "American Astronomical Society",
        "publication": "Astrophysical Journal",
        "publication_date": "1957",
        "series_number": "1",
        "volume": "125",
        "issue": "1",
        "pages": "139-152"
    }
]