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A star who's brightness changes is called a variable star.Examples are:AlgolPolarisBetelgeuse.See related link for more information.
Variable stars are stars whose brightness changes over time due to intrinsic or extrinsic factors. Intrinsic variables, like Cepheid and Mira variables, undergo changes in their own properties, such as pulsations or eruptions. Extrinsic variables, such as eclipsing binaries, have their brightness altered by external factors, like one star passing in front of another. These stars are important for studying stellar processes and measuring distances in the universe.
A pulsating star is a type of variable star that changes in brightness due to periodic expansions and contractions of its outer layers. These changes can be regular or irregular, and the star's size and temperature vary over time. Examples of pulsating stars include Cepheid variables and RR Lyrae stars.
Pulsating variable stars are stars that undergo periodic changes in brightness due to expansions and contractions in their outer layers. This rhythmic pulsation is primarily caused by instabilities in their stellar atmospheres, often linked to processes such as the ionization of helium. Common examples include Cepheid variables and RR Lyrae stars, which are crucial for measuring cosmic distances. Their predictable brightness variations make them important tools in astrophysics for understanding the scale of the universe.
The perceived brightness of an object with known brightness can be used to gauge distances. Cepheid variables are known to have a brightness directly related to their period. Which means that if we know the period of the Cepheid variable, we know what its brightness is, and can use it to gauge the distance to the stellar group the Cepheid is part of.
A star who's brightness changes is called a variable star.Examples are:AlgolPolarisBetelgeuse.See related link for more information.
A pulsating star is a type of variable star that undergoes periodic changes in brightness due to expansions and contractions in its outer layers. Examples include Cepheid variables and RR Lyrae stars, which exhibit regular cycles of brightness changes. These stars are important for measuring cosmic distances, as their pulsation periods are directly related to their intrinsic luminosities.
Variable stars are stars whose brightness changes over time due to intrinsic or extrinsic factors. Intrinsic variables, like Cepheid and Mira variables, undergo changes in their own properties, such as pulsations or eruptions. Extrinsic variables, such as eclipsing binaries, have their brightness altered by external factors, like one star passing in front of another. These stars are important for studying stellar processes and measuring distances in the universe.
A pulsating star is a type of variable star that changes in brightness due to periodic expansions and contractions of its outer layers. These changes can be regular or irregular, and the star's size and temperature vary over time. Examples of pulsating stars include Cepheid variables and RR Lyrae stars.
Pulsating variable stars are stars that undergo periodic changes in brightness due to expansions and contractions in their outer layers. This rhythmic pulsation is primarily caused by instabilities in their stellar atmospheres, often linked to processes such as the ionization of helium. Common examples include Cepheid variables and RR Lyrae stars, which are crucial for measuring cosmic distances. Their predictable brightness variations make them important tools in astrophysics for understanding the scale of the universe.
A cepheid (which take their name from prototypical stars in constellation Cepheus) is a type of star which varies or pulses over time. They are important to astronomy as they help establish a "standard candle" which helps in measurement of distance. The variation in brightness, size and spectrum is proportional to the density and size of the star; thus, the absolute magnitude can be calculated and the distance of a cepheid of a given luminance can be inferred from how quickly it changes. Hubble used this method to show that the "spiral nebulae" were in fact not close objects inside our galaxy but instead were distant galaxies.
A variable resistor can be connected in series with a light bulb in a circuit. By adjusting the resistance of the variable resistor, the current flowing through the circuit changes, affecting the brightness of the light bulb. Increasing the resistance decreases the current, resulting in lower brightness, while decreasing the resistance increases the current, leading to higher brightness.
Polaris, also known as the North Star, is a supergiant star located in the constellation Ursa Minor. It is classified as a yellow supergiant (specifically, a type F7 Ib star) and is about 2,500 times more luminous than the Sun. Polaris is a variable star, specifically a Cepheid variable, which means its brightness changes periodically. Its position nearly aligns with the North Celestial Pole, making it a crucial reference point for navigation.
The perceived brightness of an object with known brightness can be used to gauge distances. Cepheid variables are known to have a brightness directly related to their period. Which means that if we know the period of the Cepheid variable, we know what its brightness is, and can use it to gauge the distance to the stellar group the Cepheid is part of.
dependent variable
the dependent variable
the dependent variable