Analytical 2-D solutions for hydrodynamic, thermally and radiatively driven, astrophysical outflows. Applications to B stars

Kakouris, A; Moussas, X

dc.contributor.author	Kakouris, A	en
dc.contributor.author	Moussas, X	en
dc.date.accessioned	2014-03-01T01:46:24Z
dc.date.available	2014-03-01T01:46:24Z
dc.date.issued	1997	en
dc.identifier.issn	0004-6361	en
dc.identifier.uri	https://dspace.lib.ntua.gr/xmlui/handle/123456789/24892
dc.subject	hydrodynamics	en
dc.subject	stars: winds	en
dc.subject	atmospheres	en
dc.subject	flows	en
dc.subject	radiation pressure	en
dc.subject	methods: analytical	en
dc.subject	B supergiants: winds	en
dc.subject	atmospheres	en
dc.subject	mass-loss	en
dc.subject.classification	Astronomy & Astrophysics	en
dc.subject.other	OPTICALLY THIN LINES	en
dc.subject.other	STELLAR WINDS	en
dc.subject.other	EQUATORIAL PLANE	en
dc.subject.other	SOLAR-WIND	en
dc.subject.other	MODELS	en
dc.subject.other	JETS	en
dc.subject.other	ACCELERATION	en
dc.subject.other	ENVELOPES	en
dc.subject.other	FLOWS	en
dc.subject.other	DISKS	en
dc.title	Analytical 2-D solutions for hydrodynamic, thermally and radiatively driven, astrophysical outflows. Applications to B stars	en
heal.type	journalArticle	en
heal.language	English	en
heal.publicationDate	1997	en
heal.abstract	In this work, we deal with the two-dimensional problem of steady plasma outflow from rotating central astrophysical gravitational objects. Considering the stellar atmosphere optically thin and the radiative force (due to the central object's luminosity) radial, we obtain fully analytical solutions for thermally and radiatively driven outflows. The flow is helicoidal and axisymmetric and the plasma inviscid and non-polytropic. First, we generalize the Kakouris & Moussas 1996 solution imposing a generalized geometry in the flow velocity which implies differential fluid rotation. The solutions are of four types with velocity maxima either along the equator or along the polar axis of the central body. The dependence of the solutions upon the radial distance R is similar to Kakouris & Moussas 1996 case for each type of solutions. Just assuming that the radiative acceleration is a function of the distance we obtain analytical 2-D solutions for thermally and radiatively driven outflows. The inclusion of the radiative force helps the generation of the stellar wind giving higher maximum radial velocities. The velocity asymmetry between the equator and the poles varies with radial distance and it is sensitive upon the relative strength of the adopted radiative force as well as upon the degree of the fluid differential rotation. Several possible dependences of the radiative acceleration upon the radial distance are considered, and the deduction of the wind transition from a strong radiative driving to a pure non-radiative thermally driven outflow is presented by the given applications. The incorporation of the radiative force in the hydrodynamic equations is very important in massive winds of early and late type main sequence stars and evolved giants and supergiants. We present analytical 2-D solutions for thermally plus radiatively driven stellar winds and we apply one kind of them to B5I type supergiants in order to understand the observed winds of these stars under a thermal (coronal) plus a radiative mechanism of ejecting stellar plasma in the interstellar medium. Maximum outflow velocities and mass loss rates, close to the observed, are easily obtained.	en
heal.publisher	SPRINGER VERLAG	en
heal.journalName	ASTRONOMY AND ASTROPHYSICS	en
dc.identifier.isi	ISI:A1997XT42200040	en
dc.identifier.volume	324	en
dc.identifier.issue	3	en
dc.identifier.spage	1071	en
dc.identifier.epage	1082	en