Modeling the Irradiated Atmospheres of Unevolved Companions in Precataclysmic Binaries (PCB)

Pustynski, V. V.; Pustylnik, I.

doi:10.1007/978-94-010-0215-8_103

Cited by 1 publication

(5 citation statements)

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“…Increased heating results in more N iii and C iii, but the higher continuum changes the shape and hence does not reduce this problem. Combining these two considerations results in a T eff, p value of 80 000−85 000 K, comparable to the light curve analysis of Pustynski & Pustylnik (2005); Afşar & Ibanoǧlu (2008) and the revised value of BPH94. Table 3 lists the model prediction for T eq, s on the day-side of the secondary depending on T eff, p for a separation of 2.46 R and T eff, s = 3400 K. Results vary on the order of 50−100 K for 1 dex abundance changes.…”

Section: The Secondarysupporting

confidence: 77%

“…7), even though this requires an enrichment of approximately +1.5 dex in N on the primary surface. This result resembles the light-curve solution by Pustynski & Pustylnik (2005) and the new values by Afşar & Ibanoǧlu (2008).…”

Section: Primary Componentsupporting

confidence: 76%

“…Grid points with higher T eff, p , closer to the light curve analysis of Pustynski & Pustylnik (2005) and compatible with PB93, require an increase of the N abundance N by +1.5 dex and more. N is normally increased by less than one order of magnitude in AGB evolution (van Winckel 2003).…”

Section: The Primarysupporting

confidence: 58%

“…There is an ongoing effort to constrain system parameters further (e.g. more recent work by Pustynski & Pustylnik 2005;Afşar & Ibanoǧlu 2008) since the uncertainties still do not allow the evolutionary status to be pinpointed. Table 1 shows a compilation of previously derived parameters of UU Sge from Bond et al (1978), de Kool & Ritter (1993, Walton et al (1993), PB93/BPH94, Pustynski & Pustylnik (2005), Afşar & Ibanoǧlu (2008), and our results for comparison.…”

Section: Properties Of Uu Sgementioning

confidence: 99%

“…We use, like Pustynski & Pustylnik (2005), the geometry derived by PB93. Numbers in round brackets in the last column are fixed input parameters and not derived by our model.…”

Section: Properties Of Uu Sgementioning

confidence: 99%

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Structure and spectra of irradiated secondaries in close binaries

Wawrzyn¹,

Barman²,

Günther

et al. 2009

A&A

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Context. The standard stellar model atmosphere ignores the influence of external radiation. This assumption, while sufficient for most stars, fails for many short-period binaries. Aims. In setting up combined model atmospheres for close binaries, we want to constrain the parameters of both components, especially in the case of a hot primary component strongly influencing its cool secondary companion. This situation can be found after common envelope evolution (CEE). The status of both components today allows one to retrace the CEE itself. Methods. We used our stellar atmosphere code PHOENIX, which includes the effect of irradiation in its radiation transport equation, to investigate the close binary star UU Sge. We combined our calculated spectra of both components, weighted by their visible size, and adjusted the input parameters until reasonable agreement with observations is reached. Results. We derive a range of 80 000−85 000 K for the effective temperature of the primary (T eff, p ) and give a rough estimate for the primary's abundances, particularly the nitrogen enrichment. The heated day-side of the secondary has an apparent "effective" or equilibrium temperature of 24 000−26 000 K, nearly independent of its intrinsic luminosity. It shows an enhancement in nitrogen and carbon. Conclusions. The evolution of the primary and secondary stars were strongly influenced by the other's presence. Radiation from the primary on the secondary's day-side is still an important factor in understanding the secondary's atmospheric structure.

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Section: The Secondarysupporting

confidence: 77%

Section: Primary Componentsupporting

confidence: 76%

Section: The Primarysupporting

confidence: 58%

Section: Properties Of Uu Sgementioning

confidence: 99%

“…We use, like Pustynski & Pustylnik (2005), the geometry derived by PB93. Numbers in round brackets in the last column are fixed input parameters and not derived by our model.…”

Section: Properties Of Uu Sgementioning

confidence: 99%

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