Nebula Burung Hantu adalah nebula planet terletak sekitar 2.030 tahun cahaya di konstelasiUrsa Mayor.[2] Nebula ini dikenal dengan pengidentifikasi katalog Messier Object 97 (M97) and NGC 3587. Ditemukan pertama kali oleh astronomPrancisPierre Méchain pada 16 February 1781.[4] Ketika William Parsons, 3rd Earl of Rosse mengamati nebula tersebut pada tahun 1848, gambar dari ilustrasi tangannya membentuk kepala burung hantu. Kemudian nebula ini mendapatkan julukan sebagai nebula burung hantu.[5]
Usia nebula itu diperkirakan mencapai 8000 tahun.[6] Ini berjarak sekitar melingkar di penampang melintang dengan struktur internal sedikit terlihat. Terbentuk dari material yang mengalir dari angin bintang yang berasal dari pusat bintang seraya berkembang di sepanjang cabang raksasa asimtotik.[3] Nebula ini disusun dalam tiga cangkang konsentris, dengan kulit terluar sekitar 20-30% lebih besar dari kulit terdalam.[7] Penampilan dari nebula yang seperti burung hantu itu hasil dari kulit terdalam yang tidak melingkar simetris, melainkan membentuk struktur seperti barrel yang selaras dengan sudut 45° terhadap garis pengelihatan.[3]
Nebula tersebut menahan materi sekitar 0.13 kali massa matahari, termasuk hidrogen, helium, nitrogen, oksigen, dan belerang;[3] dengan kerapatannya kurang dari 100 partikel per kubik sentimeter.[7] Radius luarnya sekitar 0.91 tahun cahaya (0.28 parsek) dan mengembang dengan kecepatan 27-39 km/s ke dalam medium antarbintang sekitarnya.[3]
Besarnya 14 bintang pusat sejak telah mencapai titik balik evolusi akan memadat membentuk katai putih.[4][7] memiliki sekira 55-60% massa matahari, 41-148 kali lebih cerah dibandingkan matahari,[3] dan suhu efektif 123,000 K.[8] Bintang ini sudah berhasil diselesaikan oleh Teleskop luar angkasa Spitzer sebagai sumber titik yang tidak menunjukkan selisih karakteristik inframerah dari disk melingkar.[9]
^ abKerber, F.; et al. (September 2003), "Galactic Planetary Nebulae and their central stars. I. An accurate and homogeneous set of coordinates", Astronomy and Astrophysics, 408: 1029–1035, Bibcode:2003A&A...408.1029K, doi:10.1051/0004-6361:20031046.
^ abStanghellini, Letizia; et al. (December 2008), "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale", The Astrophysical Journal, 689 (1): 194–202, Bibcode:2003A&A...408.1029K, doi:10.1051/0004-6361:20031046.
^Per Guerrero et al (2003), the age is 12,900 × d years, where d is the distance in kpc. According to Stanghellini et al (2008), d is 0.621 kpc. Hence, the age is 12,900 × 0.621 ≈ 8,000 years.
^Capriotti, Eugene R.; Kovach, William S. (March 1968), "Effective Temperatures of the Central Stars of Planetary Nebulae", Astrophysical Journal, 151 (5): 991–995, Bibcode:1968ApJ...151..991C, doi:10.1086/149498.
^Bilíková, Jana; et al. (May 2012), "Spitzer Search for Dust Disks around Central Stars of Planetary Nebulae", The Astrophysical Journal Supplement, 200 (1): 3, Bibcode:2012ApJS..200....3B, doi:10.1088/0067-0049/200/1/3.
(Inggris) Norton, Andy. "M97 – Owl Nebula". Deep Space Videos. Brady Haran.Parameter |coauthors= yang tidak diketahui mengabaikan (|author= yang disarankan) (bantuan)
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