Spiral Bending Waves Launched at a Vertical Secular Resonance

Details Spiral Bending Waves Launched at a Vertical Secular Resonance Spiral Bending Waves Launched at a Vertical Secular Resonance

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dda....31.0701h&link_type=abstract

American Astronomical Society, DDA meeting #31, #07.01

Astronomy and Astrophysics

Astronomy

Scientific paper

The excitation of spiral bending waves at a vertical secular resonance is investigated. These nodal bending waves are launched at sites where the secondary's nodal regression rate matches the disk's rate, and they propagate in both particle and gas disks. In planet-forming environments where the local disk mass is often in excess of the secondary's mass, the resonance lies quite close to the secondary's orbit a_s, and the bending waves have a wavelength ~ (ha_s)(1/2) where h is the disk scale height. However disk stirring by the secondary or gap formation tends to weakens the wave interaction by slowing the secondary's nodal regression rate and pushing the resonance radially away. The excitation of nodal bending waves also damps out the secondary's inclination which ultimately shuts off subsequent wave generation. For instance, an Earth-mass protoplanet embedded in a minimum-mass planetesimal disk will have its inclination damped out in ~ 10(2) to 10(3) orbits if there is no gap or stirred zone, and a Jovian-mass protoplanet orbiting in a minimum-mass nebula gas disk will lose its inclination in ~ 10(3) orbits if it resides in a gap. Additional consequences of the bending-wave phenomenon in planet-forming systems shall also be discussed.

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