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Nonradial pulsation is generally occurred on stars, including intermediate-mass stars. Pulsating intermediate-mass stars can be represented by 𝛽 Cephei and SPB (slowly pulsating B) type, whose pulsations are dominantly characterized respectively as p-mode and g-mode. In this study, the p...
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id-itb.:202402017-09-27T11:42:17Z#TITLE_ALTERNATIVE# GOSALIM (NIM: 10311022); Pembimbing : Dr. Aprilia, KEVIN Indonesia Final Project INSTITUT TEKNOLOGI BANDUNG https://digilib.itb.ac.id/gdl/view/20240 Nonradial pulsation is generally occurred on stars, including intermediate-mass stars. Pulsating intermediate-mass stars can be represented by 𝛽 Cephei and SPB (slowly pulsating B) type, whose pulsations are dominantly characterized respectively as p-mode and g-mode. In this study, the pulsation of 𝛽 Cephei and SPB are analyzed using stellar model with 20 and 5 𝑀⊙ in mass, respectively. Both types are known to pulsate due to the opacity-driven 𝜅 -mechanism caused by iron at region 𝑙𝑜𝑔 𝑇 ≈ 5,3 (𝑇 ≈ 2 × 105 K). <br /> <br /> The nonradial pulsation of 𝛽 Cephei and SPB are studied better if rotation is taken into consideration. This can be done by analyzing various pulsational frequencies of pulsation modes by solving the equations of linear adiabatic nonradial pulsation using GYRE v4.0. Rotation, even in slow case, clearly affects the nonradial pulsation of both types, causing eigenfrequencies of non-rotating modes (for certain value of 𝑙 and 𝑛𝑝 or 𝑛𝑔) to be higher for retrograde modes (𝑚 =+1) or lower for prograde modes (𝑚 = −1). text |
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Nonradial pulsation is generally occurred on stars, including intermediate-mass stars. Pulsating intermediate-mass stars can be represented by 𝛽 Cephei and SPB (slowly pulsating B) type, whose pulsations are dominantly characterized respectively as p-mode and g-mode. In this study, the pulsation of 𝛽 Cephei and SPB are analyzed using stellar model with 20 and 5 𝑀⊙ in mass, respectively. Both types are known to pulsate due to the opacity-driven 𝜅 -mechanism caused by iron at region 𝑙𝑜𝑔 𝑇 ≈ 5,3 (𝑇 ≈ 2 × 105 K). <br />
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The nonradial pulsation of 𝛽 Cephei and SPB are studied better if rotation is taken into consideration. This can be done by analyzing various pulsational frequencies of pulsation modes by solving the equations of linear adiabatic nonradial pulsation using GYRE v4.0. Rotation, even in slow case, clearly affects the nonradial pulsation of both types, causing eigenfrequencies of non-rotating modes (for certain value of 𝑙 and 𝑛𝑝 or 𝑛𝑔) to be higher for retrograde modes (𝑚 =+1) or lower for prograde modes (𝑚 = −1). |
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Final Project |
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GOSALIM (NIM: 10311022); Pembimbing : Dr. Aprilia, KEVIN |
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GOSALIM (NIM: 10311022); Pembimbing : Dr. Aprilia, KEVIN #TITLE_ALTERNATIVE# |
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GOSALIM (NIM: 10311022); Pembimbing : Dr. Aprilia, KEVIN |
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GOSALIM (NIM: 10311022); Pembimbing : Dr. Aprilia, KEVIN |
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https://digilib.itb.ac.id/gdl/view/20240 |
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