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... The correlation in Figure II, together with the consideration that an increased PAH luminosit... more ... The correlation in Figure II, together with the consideration that an increased PAH luminosity is related to an increased VSG -1 0 Log[ (AFA)I,/(AFA)Q} STRUCTURES AROUND HAEBE STARS 191 j 0 FIGURE II H~ luminosity vs. ...
The Astrophysical Journal, 1992
The Astrophysical Journal, 1998
The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed ... more The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed in light of a model originally developed by Mestel for describing stellar winds ejected by rotating stars. In addition to the acceleration mechanisms of thermal expansion and stellar radiation pressure, which typically play an important role in driving the winds of low-and high-mass stars, respectively, centrifugal acceleration by a corotating magnetic Ðeld and the presence of hydromagnetic waves are taken into account. The relevance of these mechanisms for the acceleration of stellar winds from the surface of young stars is discussed in the context of growing evidence for the presence of magnetic Ðelds and surface convection in preÈmain-sequence evolutionary phases. In the particular case of Herbig Ae/Be stars, the deposition of a fraction of the convection energy in Alfve n waves seems to be required in order to explain the winds observed in these preÈmain-sequence objects. Under some simplifying assumptions, the velocity and density Ðelds around the central stellar object are derived and the emerging line proÐles are computed. A test case is discussed in which the observed line proÐles of the prototypical object AB Aur are used to constrain the model parameters, showing that the magnetic rotator model o †ers a physically consistent description of this system.
Astrophysics and Space Science Library, 1990
... The correlation in Figure II, together with the consideration that an increased PAH luminosit... more ... The correlation in Figure II, together with the consideration that an increased PAH luminosity is related to an increased VSG -1 0 Log[ (AFA)I,/(AFA)Q} STRUCTURES AROUND HAEBE STARS 191 j 0 FIGURE II H~ luminosity vs. ...
The Astrophysical Journal, 1992
The Astrophysical Journal, 1998
The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed ... more The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed in light of a model originally developed by Mestel for describing stellar winds ejected by rotating stars. In addition to the acceleration mechanisms of thermal expansion and stellar radiation pressure, which typically play an important role in driving the winds of low-and high-mass stars, respectively, centrifugal acceleration by a corotating magnetic Ðeld and the presence of hydromagnetic waves are taken into account. The relevance of these mechanisms for the acceleration of stellar winds from the surface of young stars is discussed in the context of growing evidence for the presence of magnetic Ðelds and surface convection in preÈmain-sequence evolutionary phases. In the particular case of Herbig Ae/Be stars, the deposition of a fraction of the convection energy in Alfve n waves seems to be required in order to explain the winds observed in these preÈmain-sequence objects. Under some simplifying assumptions, the velocity and density Ðelds around the central stellar object are derived and the emerging line proÐles are computed. A test case is discussed in which the observed line proÐles of the prototypical object AB Aur are used to constrain the model parameters, showing that the magnetic rotator model o †ers a physically consistent description of this system.
... The correlation in Figure II, together with the consideration that an increased PAH luminosit... more ... The correlation in Figure II, together with the consideration that an increased PAH luminosity is related to an increased VSG -1 0 Log[ (AFA)I,/(AFA)Q} STRUCTURES AROUND HAEBE STARS 191 j 0 FIGURE II H~ luminosity vs. ...
The Astrophysical Journal, 1992
The Astrophysical Journal, 1998
The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed ... more The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed in light of a model originally developed by Mestel for describing stellar winds ejected by rotating stars. In addition to the acceleration mechanisms of thermal expansion and stellar radiation pressure, which typically play an important role in driving the winds of low-and high-mass stars, respectively, centrifugal acceleration by a corotating magnetic Ðeld and the presence of hydromagnetic waves are taken into account. The relevance of these mechanisms for the acceleration of stellar winds from the surface of young stars is discussed in the context of growing evidence for the presence of magnetic Ðelds and surface convection in preÈmain-sequence evolutionary phases. In the particular case of Herbig Ae/Be stars, the deposition of a fraction of the convection energy in Alfve n waves seems to be required in order to explain the winds observed in these preÈmain-sequence objects. Under some simplifying assumptions, the velocity and density Ðelds around the central stellar object are derived and the emerging line proÐles are computed. A test case is discussed in which the observed line proÐles of the prototypical object AB Aur are used to constrain the model parameters, showing that the magnetic rotator model o †ers a physically consistent description of this system.
Astrophysics and Space Science Library, 1990
... The correlation in Figure II, together with the consideration that an increased PAH luminosit... more ... The correlation in Figure II, together with the consideration that an increased PAH luminosity is related to an increased VSG -1 0 Log[ (AFA)I,/(AFA)Q} STRUCTURES AROUND HAEBE STARS 191 j 0 FIGURE II H~ luminosity vs. ...
The Astrophysical Journal, 1992
The Astrophysical Journal, 1998
The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed ... more The winds observed in the preÈmain-sequence phase of intermediate-mass young stars are discussed in light of a model originally developed by Mestel for describing stellar winds ejected by rotating stars. In addition to the acceleration mechanisms of thermal expansion and stellar radiation pressure, which typically play an important role in driving the winds of low-and high-mass stars, respectively, centrifugal acceleration by a corotating magnetic Ðeld and the presence of hydromagnetic waves are taken into account. The relevance of these mechanisms for the acceleration of stellar winds from the surface of young stars is discussed in the context of growing evidence for the presence of magnetic Ðelds and surface convection in preÈmain-sequence evolutionary phases. In the particular case of Herbig Ae/Be stars, the deposition of a fraction of the convection energy in Alfve n waves seems to be required in order to explain the winds observed in these preÈmain-sequence objects. Under some simplifying assumptions, the velocity and density Ðelds around the central stellar object are derived and the emerging line proÐles are computed. A test case is discussed in which the observed line proÐles of the prototypical object AB Aur are used to constrain the model parameters, showing that the magnetic rotator model o †ers a physically consistent description of this system.