Model Relativistik Struktur Bintang dengan Profil Kerapatan Kuadratik
DOI:
https://doi.org/10.26418/pf.v10i2.54855Abstract
Penelitian ini dilakukan untuk mengetahui profil tekanan bintang relativistik menggunakan persamaan tekanan Oppenheimer-Volkoff yang diperoleh dari penyelesaian persamaan medan gravitasi Einstein menggunakan metode analitik. Penelitian ini menjelaskan bahwa tekanan bintang dipengaruhi oleh profil kerapatan yang berkurang secara kuadratik seiring bertambahnya jarak (r) dari inti bintang. Untuk membantu perhitungan tekanan bintang dengan profil kerapatan kuadratik, maka digunakanlah metode numerik Runge-Kutta Orde 4. Hasil penelitian ini menunjukkan bahwa tekanan maksimum terjadi di inti bintang dan semakin berkurang seiring bertambahnya jarak r dari inti bintang hingga di permukaan bintang, tekanan bernilai nol. Berdasarkan profil tekanan yang telah diperoleh, sebuah bintang relativistik harus memiliki batasan massa dan jari-jari minimum agar tetap berada dalam kesetimbangan hidrostatis. Melalui perhitungan analitik, sebuah bintang bermassa M dan berjari-jari R harus memenuhi syarat dan agar tetap stabil. Jika terdapat sebuah bintang yang tidak memenuhi syarat batas ini, maka gravitasi bintang tersebuh sangatlah besar dan tidak akan mampu diimbangi oleh tekanan dari energi yang dihasilkannya sehingga bintang tersebut mengalami keruntuhan gravitasi yang begitu cepat.
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Date: 24-05-2023
Prisma Fisika
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