Orbital period
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Understanding Orbital Periods in Various Astronomical Contexts
Orbital Periods in Sedimentary Relative Paleointensity Records
Keywords: Orbital cycles, sedimentary records, paleointensity
Research has shown that orbital cycles with periods of 100,000 years (kyr) and 41,000 years are present in some sedimentary relative paleointensity (RPI) records. These cycles have been detected through power spectral and wavelet analyses. However, the significance of these orbital periods varies across different RPI records and time intervals, suggesting that they do not have a common origin such as orbital forcing on the geodynamo. Instead, these periods are likely due to climatic contamination, as indicated by significant coherence and in-phase relationships between RPI records and benthic oxygen isotope records during certain intervals1.
Orbital Period Modulation in Close Binaries
Keywords: Close binaries, magnetic cycles, orbital period modulation
In close binary systems, observed orbital period modulations are often linked to the magnetic activity cycles of the stars. The mechanism proposed by Applegate suggests that changes in the stellar internal rotation, associated with magnetic activity, lead to variations in the gravitational quadrupole moment of the active star. This, in turn, forces changes in the orbital motion of the binary system. This interaction has been studied in detail, providing insights into the interplay between stellar rotation and magnetic field generation. For example, in the active binary RS Canum Venaticorum, torsional oscillations driven by a stellar magnetic dynamo may account for the observed orbital period behavior2.
Minimum Orbital Periods of Hydrogen-Rich Bodies
Keywords: Gas giants, brown dwarfs, minimum orbital periods
The minimum allowed orbital periods for hydrogen-rich bodies, ranging from the mass of Saturn to one solar mass, have been derived. These periods are particularly relevant for distinguishing between brown dwarfs and planets transiting host white dwarfs. For instance, orbital periods of around 100 minutes are indicative of brown dwarfs. The overall minimum period for bodies in this mass range is approximately 37 minutes, assuming the host star's density is sufficiently high3.
Determination of Orbital Periods in X-ray Binaries
Keywords: X-ray binaries, orbital ephemeris, pulsars
The binary period and orbital ephemeris of the Be X-ray binary containing the pulsar IA 1118-616 have been determined for the first time, 35 years after the source's discovery. The orbital period is found to be approximately 24 days. This determination was made using the phase connection technique during an X-ray outburst, providing a circular orbit solution consistent with the peak X-ray flux4.
Orbital Period Distribution in Cataclysmic Variables
Keywords: Cataclysmic variables, period gap, nova-like variables
The orbital period distribution of cataclysmic variables has been analyzed using the latest data compilations. Contrary to previous conclusions, the period gap is significant for nova-like variables. This analysis also explores the relationship between VY Scl stars and dwarf novae, contributing to a better understanding of these systems' orbital period characteristics5.
Orbital Period Changes in Eclipsing Cataclysmic Variables
Keywords: Eclipsing variables, period variations, magnetism
The orbital period changes in the eclipsing cataclysmic variable UX Ursae Majoris have been found to be aperiodic. This eliminates explanations such as apsidal motion or the presence of a third body. Instead, the variations may be linked to the magnetism of the secondary star, although the exact details remain unclear6.
Long-Term Orbital Period Changes in Dwarf Novae
Keywords: Dwarf novae, orbital-period change, eclipse times
A long-term study of the eclipse times in the dwarf nova WZ Sagittae reveals orbital-period changes characterized by back-and-forth wiggles with timescales of 20-50 years. These variations dominate the O–C diagram, complicating the measurement of a steady rate of orbital-period change. There may be a connection between these wiggles and the intervals between dwarf-nova eruptions7.
Conclusion
The study of orbital periods across different astronomical contexts reveals a complex interplay of factors, including magnetic activity, climatic contamination, and stellar dynamics. These insights not only enhance our understanding of specific systems but also provide broader implications for the study of orbital mechanics and stellar evolution.
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Most relevant research papers on this topic
Origin of orbital periods in the sedimentary relative paleointensity records
Orbital periods in sedimentary relative paleointensity records may not be directly caused by orbital forcing, but may be influenced by climatic 'contamination' or incomplete normalization of the records.
Orbital period modulation and magnetic cycles in close binaries
Orbital period modulation in close binaries can help distinguish between different dynamo models, potentially explaining the observed behavior of active stars like RS Canum Venaticorum.
Highly CitedMinimum Orbital Periods of H-rich Bodies
The minimum orbital period for H-rich bodies ranging in mass from Saturn's to 1 M is 37 minutes, making it easier to distinguish brown dwarfs from planets transiting white dwarfs without near-infrared or radial velocity measurements.
Finding a 24-day orbital period for the X-ray binary 1A 1118-616
The X-ray binary 1A 1118-616 has a 24-day orbital period, with a circular orbit and peak X-ray flux at MJD 54845.37, coincident with its peak outburst in 2009.
On the orbital period distribution of cataclysmic variables
The period gap is significant for nova-like variables, contrary to Verbunt's conclusion, and the VY Scl stars are related to dwarf novae.
THE ORBITAL PERIOD CHANGES OF UX URSAE MAJORIS
The orbital changes of UX Ursae Majoris are aperiodic, eliminating apsidal motion and system revolution as feasible explanations.
Orbital Period Changes in WZ Sagittae
WZ Sagittae's orbital-period changes show wiggles over 20-50 years, preventing a secure measurement of its steady rate of change.
ON THE ORBITAL PERIOD OF 70 OPHIUCHI
The orbital period of 70 Ophiuchi is 88.05 years, with a systematic difference of 0.3 km/s between two series of determinations.
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