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"The amateur astronomer's guide to the deep-sky catalogs is a single compilation of the historical and modern astronomical deep-sky catalogs. It discusses their origins, compares what's in them, explains how to interpret the data they contain, and even outlines how readers can create suitable 'custom' catalogs for their own use. The last section provides a set of three deep-sky catalogs created by the author, for observers of different levels of experience, from newcomer to expert."

"The casual sky observer's pocket guide offers an observing program for occasional amateur observers looking for some quick, fun astronomy adventures under the stars. In the real world, where time for observing is limited, the weather is seldom perfect, and expensive equipment is not an option, amateur astronomy may not be seen as a worthwhile activity. However, portable and quick-to-set-up instruments are available. A pair of binoculars or a small telescope fills the bill. And the way to make the most of these instruments is described in The casual sky observer's pocket guide.Not only does the book feature the best and brightest showpieces of the heavens; it also provides a great deal of physical and environmental data as well as lots of fascinating information and beautiful illustrations that provide a unique perspective on the many treasures within and beyond our home galaxy, the Milky Way--stars, star clusters, other galaxies, and nebulae, all within reach of binoculars or a small telescope."

"Dipelajari sifat-sifat bintang neutron statik dan berotasi dengan menggunakan pendekatan medan rata-rata relativistik dengan menggunakan parameter set NL3, TM1, FSUGold, FSUGZ03, dan FSUGZ06. Tekanan materi nuklir pada kerapatan tinggi yang diperoleh dengan menggunakan parameter set NL3 bersifat paling stiff sedangkan FSUGZ06 bersifat paling soft. Relasi massa dan jari-jari bintang neutron diperoleh dengan menyelesaikan persamaan Tollman-Oppenheimer-Volkoff (TOV) dengan input persamaan keadaan, baik dengan atau tanpa crust. Prediksi sifat-sifat bintang neutron statik berdasarkan model medan rata-rata relativistik menghasilkan massa maksimum berkisar antara 1,720 M⊙ -2,771 M⊙, sedangkan jari-jari antara 10,963 km - 13,356 km, juga kerapatan jumlah barion pada titik saturasi antara 0,145 fm−3 - 0,151 fm−3. Kerapatan jumlah barion di pusat bintang neutron pada saat massanya maksimum berkisar antara 0,668 fm−3 - 1,181 fm−3 dan kerapatan jumlah barion di daerah transisi dari materi homogen ke materi inhomogen antara 0,049 fm−3 - 0,074 fm−3, sedangkan tekanan materi nuklir pada daerah transisi tersebut berkisar antara 0,177 MeV fm−3 - 0,368 MeV fm−3. Prediksi momen inersia, momen kuadrupol, eliptisitas equator, dan amplitudo regangan gelombang gravitasi juga dipelajari.

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Static and rotating neutron star properties prediction based on relativistic mean-field (RMF) approximation using NL3, TM1, FSUGold, FSUGZ03, and FSUGZ06 parameter sets have been studied. Pressure of nuclear matter at high densities predicted by NL3 parameter set is the stiffest, but FSUGZ06 is the softest. The mass and radius relation of neutron stars are obtained by solving Tollman-Oppenheimer-Volkoff (TOV) equation where the input is equation of state of neutron star matter and with or without taking into account the neutron star crust. RMF parameter sets predict the value of maximum mass between 1,720 M⊙ - 2,771 M⊙, while the radius between 10,963 km - 13,356 km, as well as the value of barion number density at saturation point between 0,145 fm−3 -0,151 fm−3. The value of barion number density at central of neutron star with maximum mass is between 0,668 fm−3 - 1,181 fm−3 and the barion number density at transition region from core to crust is between 0,049 fm−3 - 0,074 fm−3, while the corresponding pressure is between 0,177 MeV fm−3 - 0,368 MeV fm−3. The neutron stars inertia moment, quadrupole moment, equatorial ellipticity, and gravitational-wave strain amplitude predicted by RMF model also have been discussed."

"Starburst regions in nearby and distant galaxies have a profound impact on our understanding of the early universe. This new, substantially updated and extended edition of Norbert Schulz’s unique book "From Dust to Stars" describes complex physical processes involved in the creation and early evolution of stars. It illustrates how these processes reveal themselves from radio wavelengths to high energy X-rays and gamma–rays, with special reference towards high energy signatures. Several sections devoted to key analysis techniques demonstrate how modern research in this field is pursued and new chapters are introduced on massive star formation, proto-planetary disks and observations of young exoplanets. Recent advances and contemporary research on the theory of star formation are explained, as are new observations, specifically from the three great observatories of the Spitzer Space Telescope, the Hubble Space Telescope and the Chandra X-Ray Observatory which all now operate at the same time and make high resolution space based observing in its prime. As indicated by the new title two new chapters have been included on proto-planetary disks and young exoplanets. Many more colour images illustrate attractive old and new topics that have evolved in recent years. "

"Pada tesis ini penulis melaporkan dua buah pekerjaan, yaitu i)efek boson skalar terhadap sifat-sifat bintang gelap fermionik dan ii)efek peluruhan gelap pada bintang netron dengan hyperon. Pada pekerjaan yang pertama, penulis menghitung sifat-sifat makro dari bintang seperti massa radius, momen inersia dan deformasi tidal dari bintang tersebut. Efek skalar akan membuat bintang menjadi lebih mampat. Dengan mengatur kuat interaksinya maka kita dapat melewati batas C=0.22. Pada pekerjaan yang kedua, penulis menguji usulan Fornal dan Grinstein (2019) yang menyatakan bahwa mungkin saja netron mengalami peluruhan menjadi dark matter(materi gelap) pada bintang netron dengan Hyperon. Didapati bahwa mungkin saja materi gelap ada pada inti bintang netron, namun ia hanya muncul pada kerapatan tinggi dan populasinya kecil sekali dengan populasi maksimum sekitar 0.1%.

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In this thesis two things have been done, i) the effect of the scalar boson on fermionic dark stars and ii) the dark decay effect on neutron stars with hyperon. In the first work, we calculated the macro properties of stars such as mass radius, moment of inertia and tidal deformability of the star. Scalar effects will make stars more compact. By controlling the interaction, we can exceed the C=0.22 limit. In the second work, we examined the proposals of Fornal and Grinstein (2019) which stated that perhaps neutrons experience decay into dark matter in neutron stars with Hyperon. It was found that dark matter may be present in the core of a neutron star, but it only appears at high densities and the population is very small with a maximum population of about 0.1%."

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Sebagai lanjutan dari pekerjaan Ch. Chatzisavvas et al., penelitian ini menerapkan ”kompleksitas” berdasarkan definisi menurut Lopez-Ruiz, H.L. Mancini, dan X. Calbet kepada model bintang ´ neutron (selanjutnya disebut sebagai NS, dari neutron star) yang mempunyai kerak dan inti hyperon, dengan harapan bahwa akan ditemukan sesuatu yang menarik mengenai sifat dan struktur NS. Langkah pertama adalah penyusunan densitas Lagrangian model NS berdasarkan teori medan rerata relativistik untuk mendapatkan persamaan keadaan (EoS, dari equation of state), (ρ). EoS ini selanjutnaya digunakan sebagai masukan persamaan kompleksitas yang hasilnya, yaitu nilai-nilai C didapatkan secara numerik. Diagram kompleksitas-massa NS hasil plot data keluaran menunjukkan bahwa perilaku atau bentuknya serupa dengan diagram kompleksitas-massa sistem terisolir secara umum, yaitu dengan dua minima pada kedua ujung-ujungnya dan satu maksima diantaranya. Kecilnya nilai C (untuk nilai massa maksimal teoretis) juga menunjukkan bahwa NS adalah sistem yang sangat teratur, serupa dengan kristal walaupun NS dimodelkan sebagai cairan (karena ∼99% massanya adalah materi baryon). Terakhir, penambahan kerak (crust) ke dalam EoS menunjukkan hasil bahwa kerak NS juga merupakan sistem yang teratur, dengan tingkat keteraturan yang lebih rendah dari NS secara keseluruhan.

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Continuing the work of K. Ch. Chatzisavvas and others, a measure of complexity proposed by R. Lopez-Ruiz, H.L Mancini, and X. Calbet was used to study a model of neutron star (NS) with crust ´ and hyperonic core. The author employed the relativistic-mean-field approximation theory to build the Lagrangian density model of the NS’s core and obtained the equation of state (EoS), (ρ). This EoS acts as an input for the complexity equation whose output (C-values) was obtained numerically. Plotted against the corresponding mass values, the NS’s complexity-mass diagram behaves very similarly to a complexity-phase diagram of an isolated system. If we take an NS with a theoretical maximum mass value, the results show that it’s a highly ordered system (very low C-value) - which is interesting since NS are modeled as liquids because they are mainly comprised of baryonic matter. Additionally, our results show that NS’s crust is also ordered, although not as highly as the baryonic matter.

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