Experiment Findings

Planetary Growth

February 2021

Authors:

New Mexico State University

Planets grow larger in group cycles of 186.598 million years per each NET Galactic Rotational Cycle ( Net GRC ). They grow from irregulars to Dwarf Planets, to Planets, to Gas Giants, to Proto-stars, and on to Stars over vast time periods of Billions of years.

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Article

Formation of the Planets and Asteroids: Some Difficulties of Accretion Theories

January 1984

M. M. Komesaroff

The theoretical models of planetary formation by gravitational accretion of small grains developed by Giuli (1968), Harris (1977), and Harris and Ward (1982) are examined critically in the light of the observed power-law relationship between the spin angular momentum (J) and the mass (m) of early-type main-sequence stars, planets, and asteroids, J proportional to (m exp 5/3). The ... [Show full abstract] Newtonian-mechanics explanation of this relationship is reviewed and shown to predict that most of the objects considered have actual angular velocities between 1/10 and 1/3 of the limiting value for rotational stability - a finding which is consistent with the gravitational collapse of primordial gas clouds to form stars but which forces the incorporation of unprovable or unrealistic assumptions into accretion models for the planets and especially for the asteroids.

Linking the Properties of Protoplanetary Disks and Their Host Stars in the Taurus Region

June 2019

Dallar Babaian

Protoplanetary disks are dense regions of gas and dust rotating around a young T Tauri star. As the name suggests, protoplanetary disks are where planets form. These disks can also serve as accretion material for the young central star. In this project we aim to study about 100 protoplanetary disks in the Taurus-Auriga young star forming region. The main focus of our study is the relationships ... [Show full abstract] between the spectral index, fluxes at mm-wavelengths and stellar properties, as well as the correlation between the mass of the central star and the mass of dust in the protoplanetary disk. Disk masses are inferred using previous flux observations in 0.89 mm and 1.33 mm wavelengths, as well as recent observations at a wavelength of 3 mm using The Combined Array for Research in Millimeter-wave Astronomy (CARMA). This study will allow us to refine scaling laws linking disk and stellar properties, and shed light on the origin of some of the key scaling laws recently observed from the known population of exoplanets.

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Article

A measurement of the wind speed on a brown dwarf

April 2020 · Science

High winds in an extrasolar atmosphere Brown dwarfs are objects intermediate in mass between large planets and small stars, and their atmospheres share many characteristics with gas giant planets. Wind speeds in Solar System gas giant atmospheres can be derived by comparing the planet's rotational periods in the infrared (tracing the upper atmosphere) and radio (tied to the interior). Allers et ... [Show full abstract] al. observed a nearby brown dwarf, 2MASS J10475385+2124234, and determined its infrared and radio periods. They derived an average wind speed of ∼650 meters per second in a west-to-east direction. This technique should also work for exoplanets. Science , this issue p. 169

Planetary Growth

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Formation of the Planets and Asteroids: Some Difficulties of Accretion Theories

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