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- W4243752045 abstract "In recent years cool white dwarfs have been studied for various aspects ( see e.g.Winget et al.,1987 Winget and van Horn, 1987, Koester, 1987, Llebert, 1980) and much effort has been Invested in attempts to interpret the energy distributions of these stars ( Greenstein, 1984, Zeldler-K.T. et al, 1986, Llebert et al., 1987, and others). However, it seems that in spite of these efforts the spectra in particular of the very cool objects with effective temperatures below about 6000 K are not yet fully under-stood, since they are extremely diverse and each objects needs special consideration. In addition, the analyses are extremely difficult because the principal constiuents of the atmospheres ( H, He ) and elements, which may donate the majority of electrons, are essentially invisible. Since usually only one ionlsatlon stage of an element is present, this implies that the gas pressure P g is high ( compared e.g. to the solar photosphere ), the accurate value of P g , however, cannot be determined reliably." @default.
- W4243752045 created "2022-05-12" @default.
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- W4243752045 date "1989-01-01" @default.
- W4243752045 modified "2023-10-14" @default.
- W4243752045 title "Model Atmospheres for Very Cool Hydrogen-Rich White Dwarfs" @default.
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- W4243752045 doi "https://doi.org/10.1017/s0252921100099619" @default.
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