SIMULATIONS OF WINDS OF WEAK-LINED T TAURI STARS. II. THE EFFECTS OF A TILTED MAGNETOSPHERE AND PLANETARY INTERACTIONS

Journal Article · Fri Sep 10 00:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/720/2/1262· OSTI ID:21460046

Vidotto, A A; Jatenco-Pereira, V ^[1]; Opher, M ^[2]

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1. University of Sao Paulo, Rua do Matao 1226, Sao Paulo, SP 05508-090 (Brazil)
2. George Mason University, 4400 University Drive, Fairfax, VA 22030-4444 (United States)

Based on our previous work, we investigate here the effects on the wind and magnetospheric structures of weak-lined T Tauri stars due to a misalignment between the axis of rotation of the star and its magnetic dipole moment vector. In such a configuration, the system loses the axisymmetry presented in the aligned case, requiring a fully three-dimensional (3D) approach. We perform 3D numerical magnetohydrodynamic simulations of stellar winds and study the effects caused by different model parameters, namely the misalignment angle {theta}{sub t}, the stellar period of rotation, the plasma-{beta}, and the heating index {gamma}. Our simulations take into account the interplay between the wind and the stellar magnetic field during the time evolution. The system reaches a periodic behavior with the same rotational period of the star. We show that the magnetic field lines present an oscillatory pattern. Furthermore, we obtain that by increasing {theta}{sub t}, the wind velocity increases, especially in the case of strong magnetic field and relatively rapid stellar rotation. Our 3D, time-dependent wind models allow us to study the interaction of a magnetized wind with a magnetized extrasolar planet. Such interaction gives rise to reconnection, generating electrons that propagate along the planet's magnetic field lines and produce electron cyclotron radiation at radio wavelengths. The power released in the interaction depends on the planet's magnetic field intensity, its orbital radius, and on the stellar wind local characteristics. We find that a close-in Jupiter-like planet orbiting at 0.05 AU presents a radio power that is {approx}5 orders of magnitude larger than the one observed in Jupiter, which suggests that the stellar wind from a young star has the potential to generate strong planetary radio emission that could be detected in the near future with LOFAR. This radio power varies according to the phase of rotation of the star. For three selected simulations, we find a variation of the radio power of a factor 1.3-3.7, depending on {theta} {sub t}. Moreover, we extend the investigation done in Vidotto et al. and analyze whether winds from misaligned stellar magnetospheres could cause a significant effect on planetary migration. Compared to the aligned case, we show that the timescale {tau}{sub w} for an appreciable radial motion of the planet is shorter for larger misalignment angles. While for the aligned case {tau}{sub w} {approx_equal} 100 Myr, for a stellar magnetosphere tilted by {theta}{sub t} = 30{sup 0}, {tau} {sub w} ranges from {approx}40 to 70 Myr for a planet located at a radius of 0.05 AU. Further reduction on {tau}{sub w} might occur for even larger misalignment angles and/or different wind parameters.

• OSTI ID: 21460046
• Journal Information: Astrophysical Journal, Vol. 720, Issue 2; Other Information: DOI: 10.1088/0004-637X/720/2/1262; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COMPUTERIZED SIMULATION
EMISSION
JUPITER PLANET
MAGNETIC DIPOLE MOMENTS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MAIN SEQUENCE STARS
ROTATION
STAR EVOLUTION
STELLAR MAGNETOSPHERES
STELLAR WINDS
T TAURI STARS
TIME DEPENDENCE
ATMOSPHERES
BINARY STARS
DIPOLE MOMENTS
ERUPTIVE VARIABLE STARS
EVOLUTION
FLUID MECHANICS
HYDRODYNAMICS
MAGNETIC MOMENTS
MECHANICS
MOTION
PLANETS
SIMULATION
STARS
STELLAR ACTIVITY
STELLAR ATMOSPHERES
VARIABLE STARS