Ade 2013 Planck 2013年的结果

主要内容:
Planck卫星的观测放出了一大批结果，20多篇的系列文章，可能没有别的这么大的手笔了吧。都投到了A＆A。这是它们的Overview。

总体上来说就像Planck发射的目标一样，得到了更加精细的结果。偏振数据还没放出来。

宇宙学参数有所改动（WMAP每次出新结果也改动了的）：宇宙年龄比137长了点儿 138.2亿年，哈伯常数小了点儿H0 = (67+- 1.2) km s^-1Mpc^-1，暗能量的比例少了些，Omega_lambda:
 0.67+0.027-0.023 (68 % CL).

精彩摘抄:

所有文章的概述，那些文章干了啥。本文就主要是概述，列举了主要结果：frequency map， component map， power spectra， parameters

全天图，包括银河系等所有的源。

各波段的全天图

仅有微波背景辐射的全天图，可见比COBE和WMAP都更精细。

角向功率谱

功率密度谱

功率密度谱，和别的结果放在一张图上

宇宙学参数的结果

文章信息:

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· arXiv e-print (arXiv:1303.5062)

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Title:		Planck 2013 results. I. Overview of products and scientific results
Authors:		Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartelmann, M.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bowyer, J. W.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cappellini, B.; Cardoso, J.-F.; Carr, R.; Casale, M.;Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.-R.; Chen, X.; Chiang, L.-Y; Chiang, H. C.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J.-M.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.;Falgarone, E.; Finelli, F.; Foley, S.; Forni, O.; Frailis, M.; Franceschi, E.; Freschi, M.; Fromenteau, S.; Gaier, T. C.; Galeotta, S.; Gallegos, J.; Gandolfo, B.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;Gregorio, A.; Gruppuso, A.; Haissinski, J.; Hansen, F. K.; Hanson, D.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;Huffenberger, K. M.; Jaffe, T. R.; Jaffe, A. H.; Jewell, J.; Jones, W. C.; Juvela, M.; Kangaslahti, P.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.;Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Leroy, C.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lowe, S.; Lubin, P. M.; Macías-Pérez, J. F.;Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McDonald, A.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.;Migliaccio, M.; Miniscalco, R.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; North, C.; Noviello, F.;Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, D.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.;Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.;Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Salerno, E.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Smoot, G. F.;Spencer, L. D.; Starck, J.-L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Tavagnacco, D.; Taylor, D.; Terenzi, L.; Texier, D.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;Tuovinen, J.; Türler, M.; Tuttlebee, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Watson, R.; Watson, C.; White, M.; White, S. D. M.; Wilkinson, A.; Yvon, D.;Zacchei, A.; Zonca, A.
Publication:		eprint arXiv:1303.5062
Publication Date:		03/2013
Origin:		ARXIV
Keywords:		Astrophysics - Cosmology and Extragalactic Astrophysics
Bibliographic Code:		2013arXiv1303.5062P

Abstract

The ESA's Planck satellite, dedicated to studying the early universe, was launched on May 2009 and has been surveying the microwave and submillimetre sky since August 2009. In March 2013, ESA and the Planck Collaboration publicly released the initial cosmology products based on the first 15.5 months of Planck operations, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper describes the mission and its performance, and gives an overview of the processing and analysis of the data, the characteristics of the data, the main scientific results, and the science data products and papers in the release. Scientific results include robust support for the standard, six parameter LCDM model of cosmology and improved measurements for the parameters that define this model, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for some of these parameters and others derived from them are significantly different from those previously determined. Several large scale anomalies in the CMB temperature distribution detected earlier by WMAP are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at 25 sigma. Planck finds no evidence for non-Gaussian statistics of the CMB anisotropies. There is some tension between Planck and WMAP results; this is evident in the power spectrum and results for some of the cosmology parameters. In general, Planck results agree well with results from the measurements of baryon acoustic oscillations. Because the analysis of Planck polarization data is not yet as mature as the analysis of temperature data, polarization results are not released. We do, however, illustrate the robust detection of the E-mode polarization signal around CMB hot- and cold-spots.

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Bibtex entry for this abstract   Preferred format for this abstract (see Preferences) 在宇宙学方面的结果（还在别的领域也有结果的）

With the Planck data, we: (a) firmly establish a deviation from scale invariance for primordial matter perturbations, a key indicator of cosmic inflation; (b) detect with high significance lensing of the CMB by intervening matter, providing evidence for dark energy from the CMB alone; (c) find no evidence for significant deviations from Gaussianity in the statistics of CMB anisotropies; (d) find a low value of the Hubble constant, in tension with the value derived from the standard distance ladder; (e) find a deficit of power at low-`s with respect to our best-fit model; (f) confirm the anomalies at large angular scales first detected by WMAP; and (g) establish the number of neutrino species at three.

Cepheid variable star为什么被翻译成造父变星

昨天彭老师给我们上完课，一起走在回宾馆的路上，我就问到一直奇怪的问题：Cepheid variable star为什么被翻译成造父变星？
我还没问完呢，他就说是戴文赛先生翻译的，因为我们古代命名了一颗星叫造父星，而它是一个典型的Cepheid variable star，于是这种星就叫造父变星。
彭老师真是天文活字典啊，还包括八卦。。。

Remillard 2006 黑洞双星的X射线辐射

主要内容:


精彩摘抄:

一些黑洞双星的大小

20个确认了的黑洞

Q形图

其中某个的光变和谱

高频QPO

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Title:		X-Ray Properties of Black-Hole Binaries
Authors:		Remillard, Ronald A.; McClintock, Jeffrey E.
Publication:		Annual Review of Astronomy & Astrophysics, vol. 44, Issue 1, pp.49-92 (Annual Reviews Homepage)
Publication Date:		09/2006
Origin:		ARAA
DOI:		10.1146/annurev.astro.44.051905.092532
Bibliographic Code:		2006ARA&A..44...49R

Abstract

We review the properties and behavior of 20 X-ray binaries that contain a dynamically-confirmed black hole, 17 of which are transient systems. During the past decade, many of these transient sources were observed daily throughout the course of their typically year-long outburst cycles using the large-area timing detector aboard the Rossi X-Ray Timing Explorer. The evolution of these transient sources is complex. Nevertheless, there are behavior patterns common to all of them as we show in a comprehensive comparison of six selected systems. Central to this comparison are three X-ray states of accretion, which are reviewed and defined quantitatively. We discuss phenomena that arise in strong gravitational fields, including relativistically-broadened Fe lines, high-frequency quasi-periodic oscillations (100 450 Hz), and relativistic radio and X-ray jets. Such phenomena show us how a black hole interacts with its environment, thereby complementing the picture of black holes that gravitational wave detectors will provide. We sketch a scenario for the potential impact of timing/spectral studies of accreting black holes on physics and discuss a current frontier topic, namely, the measurement of black hole spin.

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Mirabel 1998 银河系中的微类星体

主要内容:


精彩摘抄:

看到了视超光速运动  GRS1915+105

著名的图就是来自这篇文章

文章信息:

Progress

Nature 392, 673-676 (16 April 1998) | doi:10.1038/33603

Microquasars in our Galaxy

I. F. Mirabel¹ & L. F. Rodríguez²

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Abstract

Microquasars are stellar-mass black holes in our Galaxy that mimic, on a smaller scale, many of the phenomena seen in quasars. Their discovery opens the way for a new understanding of the connection between the accretion of matter onto black holes and the origin of the relativistic jets observed in remote quasars.

Discovered more than 30 years ago, quasars remain some of the most mysterious objects in the Universe. It is widely believed that they are powered by black holes of several million solar masses or more that lie at the centres of remote galaxies. Their luminosities are much larger than ordinary galaxies like the Milky Way, yet originate from regions smaller than the size of the Solar System. Occasionally, quasars spout jets of gas that appear to move on the plane of the sky with velocities exceeding that of light (that is, with superluminal velocities). The extreme distance of quasars introduces many uncertainties into the interpretation of the source of energy and the nature of the ejecta that appear to be moving with superluminal speeds.

The recent finding in our own Galaxy of microquasars^{1, 2, 3, 4}, a class of objects that mimics — on scales millions of times smaller — the properties of quasars, has opened new perspectives for the astrophysics of black holes (seeFig. 1). These scaled-down versions of quasars are believed to be powered by spinning black holes⁵ but with masses of up to a few tens times that of the Sun. The word microquasar was chosen to suggest that the analogy with quasars is more than morphological, and that there is an underlying unity in the physics of accreting black holes over an enormous range of scales, from stellar-mass black holes in binary stellar systems, to supermassive black holes at the centre of distant galaxies. As the characteristic times in the flow of matter onto a black hole are proportional to its mass, variations with intervals of minutes in a microquasar correspond to analogous phenomena with durations of thousands of years in a quasar of 10⁹ solar masses, which is much longer than a human lifetime. Therefore, variations with minutes of duration in microquasars could be sampling phenomena that we have not been able to study in quasars.

Mirabel 1999 银河系中的相对论性喷流

主要内容:




精彩摘抄:

当时（1999年）就这几个源，而且都是大角度指向的。

theta的含义。

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Title:		Sources of Relativistic Jets in the Galaxy
Authors:		Mirabel, I. F.; Rodríguez, L. F.
Affiliation:		AA(Centre d'Études de Saclay, CEA/DSM/DAPNIA/Sap, Gif-sur-Yvette, F-91191 France; and Instituto de Astronomía y Física del Espacio C.C. 67, Suc. 28. 1428, Buenos Aires, Argentina mirabel@discovery.saclay.cea.fr), AB(Instituto de Astronomía, UNAM, Apdo. 04510 México, México D.F., Postal 70-264 luisfr@astrosmo.unam.mx)
Publication:		Annual Review of Astronomy and Astrophysics, Vol. 37, pp. 409-443. (Annual Reviews Homepage)
Publication Date:		00/1999
Origin:		ARA&A
Keywords:		RADIO CONTINUUM STARS, SUPERLUMINAL MOTION, X-RAYS BINARIES
DOI:		10.1146/annurev.astro.37.1.409
Bibliographic Code:		1999ARA&A..37..409M

Abstract

Black holes of stellar mass and neutron stars in binary systems are first detected as hard X-ray sources using high-energy space telescopes. Relativistic jets in some of these compact sources are found by means of multiwavelength observations with ground-based telescopes. The X-ray emission probes the inner accretion disk and immediate surroundings of the compact object, whereas the synchrotron emission from the jets is observed in the radio and infrared bands, and in the future could be detected at even shorter wavelengths. Black-hole X-ray binaries with relativistic jets mimic, on a much smaller scale, many of the phenomena seen in quasars and are thus called microquasars. Because of their proximity, their study opens the way for a better understanding of the relativistic jets seen elsewhere in the Universe. From the observation of two-sided moving jets it is inferred that the ejecta in microquasars move with relativistic speeds similar to those believed to be present in quasars. The simultaneous multiwavelength approach to microquasars reveals in short timescales the close connection between instabilities in the accretion disk seen in the X-rays, and the ejection of relativistic clouds of plasma observed as synchrotron emission at longer wavelengths. Besides contributing to a deeper understanding of accretion disks and jets, microquasars may serve in the future to determine the distances of jet sources using constraints from special relativity, and the spin of black holes using general relativity.

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