A formula for calculating the rotational period of planet or star

2021 ◽  
Author(s):  
xiaozhong zhai
Keyword(s):  
Rotation Period ◽  
Gravitational Acceleration ◽  
Orbital Velocity ◽  
Rotational Period

Abstract This paper reports a formula for calculating the rotation period of planet or star. The rotational radius, the orbital velocity and the gravitational acceleration at its surface, the three factors, determine the rotational period of planet or star.

scholarly journals A formula for calculating the rotational period of planet or star

2021 ◽  
Author(s):  
xiaozhong zhai
Keyword(s):  
Rotation Period ◽  
Gravitational Acceleration ◽  
Orbital Velocity ◽  
Rotational Period

Abstract This paper reports a formula for calculating the rotation period of planet or star. The rotational radius, the orbital velocity and the gravitational acceleration at its surface, the three factors, determine the rotational period of planet or star.

scholarly journals Experimental Comparison of Radon Domain Approaches for Resident Space Object’s Parameter Estimation

Sensors ◽  
2021 ◽  
Vol 21 (4) ◽  
pp. 1298
Author(s):  
Selenia Ghio ◽  
Marco Martorella ◽  
Daniele Staglianò ◽  
Dario Petri ◽  
Stefano Lischi ◽  
...  
Keyword(s):  
Experimental Data ◽  
Rotation Period ◽  
Research Topic ◽  
Experimental Comparison ◽  
Rotational Period ◽  
Space Objects ◽  
Resident Space Objects ◽  
The Moment ◽  
Inverse Radon Transform ◽  
Inverse Radon

The fast and uncontrolled rise of the space objects population is threatening the safety of space assets. At the moment, space awareness solutions are among the most calling research topic. In fact, it is vital to persistently observe and characterize resident space objects. Instrumental highlights for their characterization are doubtlessly their size and rotational period. The Inverse Radon Transform (IRT) has been demonstrated to be an effective method for this task. The analysis presented in this paper has the aim to compare various approaches relying on IRT for the estimation of the object’s rotation period. Specifically, the comparison is made on the basis of simulated and experimental data.

scholarly journals Determination of the rotational period of the comet 29P/Schwassmann-Wachmann-1 using dynamics of the dust structures (jets) in the coma

2012 ◽  
Vol 10 (H16) ◽  
pp. 176-176
Author(s):  
Aleksandra Ivanova ◽  
Viktor Afanasiev ◽  
Pavlo Korsun ◽  
Aleksandr Baransky ◽  
Maksim Andreev ◽  
...  
Keyword(s):  
Digital Filters ◽  
Cross Correlation ◽  
Rotation Period ◽  
Correlation Method ◽  
Photometric Data ◽  
Rotational Period ◽  
Water Ice ◽  
Ice Sublimation ◽  
Made In

AbstractWe present analysis of the photometric data of the distant comet 29P/Schwassmann-Wachmann-1, obtained at the 6-m BTA telescope (SAO RAS, Russia) and at the 2-meter telescope Zeiss-2000 (ICAMER, KB). The comet shows significant jets activity at large heliocentric distances, beyond the zone of water ice sublimation. Various digital filters were applied to increase the contrast of the jets and separate them. The rotation period of the nucleus was derived using cross-correlation method. The value of the rotation period is 12.1 ± 1.2 days for observations made in 2008 and 11.7 ± 1.5 days for observations made in 2009.

scholarly journals The circumstellar environment of σ Orionis E

1994 ◽  
Vol 162 ◽  
pp. 171-172
Author(s):  
C. Ian Short ◽  
C. T. Bolton
Keyword(s):  
Rotation Period ◽  
Circumstellar Matter ◽  
Published Data ◽  
Rotational Period ◽  
High Quality ◽  
Chemically Peculiar ◽  
Be Star ◽  
Circumstellar Environment

The light and spectrum of the magnetic, chemically peculiar Be star σ Orionis E (=HD 37479) vary with the rotational period of 1.19081 d because of the effects of inhomogeneities in the photosphere and circumstellar matter (Walborn and Hesser 1976, Landstreet and Borra 1978, Hunger 1974). In this paper, we describe a model for the distribution of the Hα emitting material in the magnetosphere based on analysis of 24 high quality spectra covering the entire rotation period and published data from other sources.

scholarly journals The History of Activity of the Sun and its Rotational Period on the ZAMS

1991 ◽  
Vol 130 ◽  
pp. 288-293
Author(s):  
Kazimierz Stępień
Keyword(s):  
Solar Activity ◽  
Initial Period ◽  
Rotation Period ◽  
The Sun ◽  
Emission Flux ◽  
Rotational Period ◽  
X Ray ◽  
The Earth ◽  
Evolution Of Life ◽  
History Of

AbstractThe rotation period of the Sun after it reached ZAMS is estimated from the present rotation rate, average X-ray emission flux and average calcium emission flux. Taking into account all existing uncertainties it is concluded that this initial period was within the range 1–9 days, with the most probable value 2–3 days. Possible influence of the solar activity on evolution of life on the Earth is briefly discussed.

scholarly journals Planetary tidal interactions and the rotational evolution of low-mass stars

2018 ◽  
Vol 619 ◽  
pp. A80 ◽  
Author(s):  
F. Gallet ◽  
E. Bolmont ◽  
J. Bouvier ◽  
S. Mathis ◽  
C. Charbonnel
Keyword(s):  
Angular Momentum ◽  
Main Sequence ◽  
Open Cluster ◽  
Rotation Period ◽  
Rotational Period ◽  
Low Mass Stars ◽  
General Behaviour ◽  
Period Distribution ◽  
Rotational Evolution ◽  
Low Mass

Context. The surface angular velocity evolution of low-mass stars is now globally understood and the main physical mechanisms involved in it are observationally quite constrained. However, while the general behaviour of these mechanisms is grasped, their theoretical description is still under ongoing work. This is the case, for instance, about the description of the physical process that extracts angular momentum from the radiative core, which could be described by several theoretical candidates. Additionally, recent observations showed anomalies in the rotation period distribution of open cluster, main sequence, early K-type stars that cannot be reproduced by current angular momentum evolution models. Aims. In this work, we study the parameter space of star-planet system’s configurations to investigate if including the tidal star-planet interaction in angular momentum evolution models could reproduce the anomalies of this rotation period distribution. Methods. To study this effect, we use a parametric angular momentum evolution model that allows for core-envelope decoupling and angular momentum extraction by magnetized stellar wind that we coupled to an orbital evolution code where we take into account the torque due to the tides raised on the star by the planet. We explore different stellar and planetary configurations (stellar mass from 0.5 to 1.0 M⊙ and planetary mass from 10 M⊕ to 13 Mjup) to study their effect on the planetary orbital and stellar rotational evolution. Results. The stellar angular momentum is the most impacted by the star-planet interaction when the planet is engulfed during the early main sequence phase. Thus, if a close-in Jupiter-mass planet is initially located at around 50% of the stellar corotation radius, a kink in the rotational period distribution opens around late and early K-type stars during the early main sequence phase. Conclusions. Tidal star-planet interactions can create a kink in the rotation period distribution of low-mass stars, which could possibly account for unexpected scatter seen in the rotational period distribution of young stellar clusters.

scholarly journals The first observed stellar occultations by the irregular satellite Phoebe (Saturn IX) and improved rotational period

2019 ◽  
Vol 492 (1) ◽  
pp. 770-781
Author(s):  
A R Gomes-Júnior ◽  
M Assafin ◽  
F Braga-Ribas ◽  
G Benedetti-Rossi ◽  
B E Morgado ◽  
...  
Keyword(s):  
3D Model ◽  
Rotation Period ◽  
Light Curves ◽  
Rotational Period ◽  
Shape Model ◽  
Stellar Occultation ◽  
Stellar Occultations ◽  
The Difference ◽  
The Moment ◽  
Gaia Dr2

ABSTRACT We report six stellar occultations by Phoebe (Saturn IX), an irregular satellite of Saturn, obtained between mid-2017 and mid-2019. The 2017 July 6 event was the first stellar occultation by an irregular satellite ever observed. The occultation chords were compared to a 3D shape model of the satellite obtained from Cassini observations. The rotation period available in the literature led to a sub-observer point at the moment of the observed occultations where the chords could not fit the 3D model. A procedure was developed to identify the correct sub-observer longitude. It allowed us to obtain the rotation period with improved precision compared to the currently known value from literature. We show that the difference between the observed and the predicted sub-observer longitude suggests two possible solutions for the rotation period. By comparing these values with recently observed rotational light curves and single-chord stellar occultations, we can identify the best solution for Phoebe’s rotational period as 9.27365 ± 0.00002 h. From the stellar occultations, we also obtained six geocentric astrometric positions in the ICRS as realized by the Gaia DR2 with uncertainties at the 1-mas level.

Rotational Characteristics of the Green Solar Corona: 1947-1991

1994 ◽  
Vol 144 ◽  
pp. 139-141 ◽  
Author(s):  
J. Rybák ◽  
V. Rušin ◽  
M. Rybanský
Keyword(s):  
Solar Corona ◽  
World Wide ◽  
Rotation Period ◽  
Original Data ◽  
Coronal Emission ◽  
Time Intervals ◽  
Data Set ◽  
The World ◽  
Coronal Emission Line ◽  
Homogeneous Data

AbstractFe XIV 530.3 nm coronal emission line observations have been used for the estimation of the green solar corona rotation. A homogeneous data set, created from measurements of the world-wide coronagraphic network, has been examined with a help of correlation analysis to reveal the averaged synodic rotation period as a function of latitude and time over the epoch from 1947 to 1991.The values of the synodic rotation period obtained for this epoch for the whole range of latitudes and a latitude band ±30° are 27.52±0.12 days and 26.95±0.21 days, resp. A differential rotation of green solar corona, with local period maxima around ±60° and minimum of the rotation period at the equator, was confirmed. No clear cyclic variation of the rotation has been found for examinated epoch but some monotonic trends for some time intervals are presented.A detailed investigation of the original data and their correlation functions has shown that an existence of sufficiently reliable tracers is not evident for the whole set of examinated data. This should be taken into account in future more precise estimations of the green corona rotation period.

On the Configuration of the Magnetic Field of β CrB

1976 ◽  
Vol 32 ◽  
pp. 613-622
Author(s):  
I.A. Aslanov ◽  
Yu.S. Rustamov
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Radial Velocity ◽  
Magnetic Field Strength ◽  
Complex Shape ◽  
Rotation Period ◽  
Field Variation ◽  
Magnetic Field Variation ◽  
Secular Variations ◽  
The Magnetic Field

SummaryMeasurements of the radial velocities and magnetic field strength of β CrB were carried out. It is shown that there is a variability with the rotation period different for various elements. The curve of the magnetic field variation measured from lines of 5 different elements: FeI, CrI, CrII, TiII, ScII and CaI has a complex shape specific for each element. This may be due to the presence of magnetic spots on the stellar surface. A comparison with the radial velocity curves suggests the presence of a least 4 spots of Ti and Cr coinciding with magnetic spots. A change of the magnetic field with optical depth is shown. The curve of the Heffvariation with the rotation period is given. A possibility of secular variations of the magnetic field is shown.

The Scanning Electron Microscopic Observation of the Vestibular Sensory Epithelia

1969 ◽  
Vol 27 ◽  
pp. 40-41
Author(s):  
D.J. Lim ◽  
W.C. Lane
Keyword(s):  
Semicircular Canals ◽  
Electron Microscopic Observation ◽  
Gravitational Acceleration ◽  
Electron Microscopic ◽  
Sensory Epithelia ◽  
Scanning Electron Microscopic ◽  
Vestibular Sensory Epithelia ◽  
And Function ◽  
Sand Piles ◽  
Active Investigation

The morphology and function of the vestibular sensory organs has been extensively studied during the last decade with the advent of electron microscopy and electrophysiology. The opening of the space age also accelerated active investigation in this area, since this organ is responsible for the sensation of balance and of linear, angular and gravitational acceleration.The vestibular sense organs are formed by the saccule, utricle and three ampullae of the semicircular canals. The maculae (sacculi and utriculi) have otolithic membranes on the top of the sensory epithelia. The otolithic membrane is formed by a layer of thick gelatin and sand-piles of calcium carbonate crystals (Fig.l).

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