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Related Concept Videos

Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
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Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
Atomic Nuclei: Larmor Precession Frequency01:11

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Reduced Mass Coordinates: Isolated Two-body Problem01:12

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Bringing the Visible Universe into Focus with Robo-AO
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RR-Lyrae-type pulsations from a 0.26-solar-mass star in a binary system.

G Pietrzyński1, I B Thompson, W Gieren

  • 1Departamento de Astronomìa, Universidad de Concepción, Casilla 160-C, Concepciòn, Chile. pietrzyn@astrouw.edu.pl

Nature
|April 7, 2012
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Summary

A peculiar RR Lyrae star was found to be a low-mass object in an eclipsing binary system. This finding suggests that while rare, such binary systems can mimic true RR Lyrae stars, impacting stellar population studies.

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Area of Science:

  • * Astronomy and Astrophysics
  • * Stellar Evolution
  • * Galactic Archaeology

Background:

  • * RR Lyrae stars are crucial for determining galactic ages and extragalactic distances.
  • * RR Lyrae stars are typically old, low-mass pulsating stars.
  • * Understanding the mass of RR Lyrae stars is essential for accurate astrophysical models.

Purpose of the Study:

  • * To determine the mass of the RR Lyrae star OGLE-BLG-RRLYR-02792.
  • * To investigate the evolutionary path of stars within eclipsing binary systems.
  • * To assess the impact of binary systems on the use of RR Lyrae stars as distance indicators.

Main Methods:

  • * Analysis of photometric data from an eclipsing binary system.
  • * Stellar evolution modeling to explain observed properties.
  • * Comparison of the pulsator's characteristics with classical RR Lyrae star models.

Main Results:

  • * OGLE-BLG-RRLYR-02792 has a mass of 0.26 solar masses, inconsistent with classical RR Lyrae stars.
  • * The system's properties are explained by the evolution of a binary system with initial masses of 1.0 M☉ and 0.8 M☉.
  • * The observed pulsator is in a short-lived phase mimicking RR Lyrae stars due to mass exchange.

Conclusions:

  • * The studied object is not a classical RR Lyrae star but an evolved binary system.
  • * Binary interlopers are estimated to contaminate only 0.2% of RR Lyrae stars.
  • * Distances derived from RR Lyrae stars are unlikely to be significantly affected by such binary systems.