List of brightest stars: Difference between revisions

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Revision as of 22:52, 23 September 2016 editTarl N. (talk \| contribs)Extended confirmed users, Pending changes reviewers, Rollbackers12,547 edits Undid revision 740870882 by Arianewiki1 (talk) I didn't see any such proof on the talk page. And we still need a reference for the statement about which magnitude is used.← Previous edit		Revision as of 23:34, 23 September 2016 edit undoArianewiki1 (talk \| contribs)Extended confirmed users7,591 edits Undid revision 740881056 by Tarl N. (talk) Removing this leaves the quoted variable star magnitudes unexplained. The proviso already formally says "not perfectly defined for the following reasons."Next edit →
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	* New or more accurate ], standard filters, or adopting differing methods using standard stars can measure stellar magnitudes slightly differently. This can change the apparent order of lists of bright stars. The table shows V magnitudes, and is measured using a ] that closely approximates human vision. However, other kinds of magnitude systems do exist based on different wavelengths, some well away from the distribution of the visible wavelengths of light, and this affects the assumed apparent brightness. This generally explains the cause of magnitude variance in the literature.		* New or more accurate ], standard filters, or adopting differing methods using standard stars can measure stellar magnitudes slightly differently. This can change the apparent order of lists of bright stars. The table shows V magnitudes, and is measured using a ] that closely approximates human vision. However, other kinds of magnitude systems do exist based on different wavelengths, some well away from the distribution of the visible wavelengths of light, and this affects the assumed apparent brightness. This generally explains the cause of magnitude variance in the literature.
	* There are sometimes small statistical variations in measured magnitudes; however, for most of the brightest stars, accurate ] means brightness stays unchanged. These particular stars are sometimes called ], which appear in the ] like the FK4, FK5 or FK6.		* There are sometimes small statistical variations in measured magnitudes; however, for most of the brightest stars, accurate ] means brightness stays unchanged. These particular stars are sometimes called ], which appear in the ] like the FK4, FK5 or FK6.
	* Some stars, like ] and ], are ]s, changing their magnitude over days, months or years. In the table, the range of variation is indicated with <small>var</small>.		* Some stars, like ] and ], are ]s, changing their magnitude over days, months or years. In the table, the range of variation is indicated with <small>var</small>. Magnitudes are expressed within the table are either when the stars are at maximum, or for the red variable stars, they are based on the mean brightness of the star when it is near maximum, which is general estimated over many observed light-curve cycles, sometimes lasting centuries.
	* The source of magnitudes cited in this list is the Misplaced Pages articles referenced - this list is simply a catalog of what Misplaced Pages itself documents.		* The source of magnitudes cited in this list is the Misplaced Pages articles referenced - this list is simply a catalog of what Misplaced Pages itself documents.
	* The source of Proper Names in this list is the .		* The source of Proper Names in this list is the .

Revision as of 23:34, 23 September 2016

This article is about apparent magnitude. For absolute magnitude, see List of most luminous stars.

This is a list of the brightest naked eye stars to +2.50 magnitude, as determined by their maximum, total or combined apparent visual magnitudes as seen from Earth. Although several of the brightest stars are also known close binary or multiple star systems, they do appear to the naked eye as single stars. The given list below combines/adds the magnitudes of bright individual components.

Measurement

Apparent visual magnitudes of the brightest star can also be compared to non-stellar objects in our Solar System. Here the maximum visible magnitudes above the brightest star, Sirius (−1.46), are as follows. Excluding the Sun, the brightest objects are the Moon (−12.7), Venus (−4.89), Jupiter (−2.94), Mars (−2.91), Mercury (−2.45), and Saturn (−0.49).

Any exact order of the visual brightness of stars is not perfectly defined for the following reasons:

Stellar brightness were traditionally based on the apparent visual magnitude as perceived by the human eye, from the brightest stars of 1st magnitude to the faintest at 6th magnitude. Since the invention of the telescope and the discovery of double or binary stars meant that star brightness could be expressed as either individual (separate) or total (combined). The table is ordered by combined magnitude of all components that appear to the naked eye as if it were a single star, with the magnitudes of any individual components bright enough to make a detectable contribution included in parentheses. For example, the total or combined magnitude of the double star Alpha Centauri is −0.27, while its two component stars have magnitudes of +0.01 and +1.33.
New or more accurate photometry, standard filters, or adopting differing methods using standard stars can measure stellar magnitudes slightly differently. This can change the apparent order of lists of bright stars. The table shows V magnitudes, and is measured using a specific filter that closely approximates human vision. However, other kinds of magnitude systems do exist based on different wavelengths, some well away from the distribution of the visible wavelengths of light, and this affects the assumed apparent brightness. This generally explains the cause of magnitude variance in the literature.
There are sometimes small statistical variations in measured magnitudes; however, for most of the brightest stars, accurate photometry means brightness stays unchanged. These particular stars are sometimes called standard stars, which appear in the Catalogues of Fundamental Stars like the FK4, FK5 or FK6.
Some stars, like Betelgeuse and Antares, are variable stars, changing their magnitude over days, months or years. In the table, the range of variation is indicated with var. Magnitudes are expressed within the table are either when the stars are at maximum, or for the red variable stars, they are based on the mean brightness of the star when it is near maximum, which is general estimated over many observed light-curve cycles, sometimes lasting centuries.
The source of magnitudes cited in this list is the Misplaced Pages articles referenced - this list is simply a catalog of what Misplaced Pages itself documents.
The source of Proper Names in this list is the International Astronomical Union's Catalog of Star Names.

Main table of the brightest stars

V Mag. (m_V)	Proper name	Bayer designation	Distance (ly)	Spectral class
0.000−26.74	Sun		0.000 015 813	G2 V
0.001−1.46	Sirius	α CMa	0008.6	A1 V, DA2
0.003−0.74	Canopus	α Car	0310	A9 II
0.004−0.27 (0.01 + 1.33)	-	α Cen	0004.4	G2 V, K1 V
0.005−0.05	Arcturus	α Boo	0037	K0 III
0.03 (−0.02 - 0.07var)	Vega	α Lyr	0025	A0 Va
0.08 (0.03 - 0.16var)	Capella	α Aur	0042	K0 III, G1 III
0.13 (0.05 - 0.18var)	Rigel	β Ori	0860	B8 Ia
0.34	Procyon	α CMi	0011	F5 IV-V
0.46 (0.40 - 0.46var)	Achernar	α Eri	0140	B6 Vep
0.50 (0.2 - 1.2var)	Betelgeuse	α Ori	0640	M2 Iab
0.61	Hadar	β Cen	0350	B1 III
0.76	Altair	α Aql	0017	A7 V
0.76 (1.33 + 1.73)	Acrux	α Cru	0320	B0.5 IV, B1 V
0.86 (0.75 - 0.95var)	Aldebaran	α Tau	0065	K5 III
0.96 (0.6 - 1.6var)	Antares	α Sco	0600	M1.5 Iab, B3 V
0.97 (0.97 - 1.04var)	Spica	α Vir	0260	B1 III-IV, B2 V
1.14	Pollux	β Gem	0034	K0 III
1.16	Fomalhaut	α PsA	0025	A3 V
1.25 (1.21 - 1.29var)	Deneb	α Cyg	2,600	A2 Ia
1.25 (1.23 - 1.31var)	Mimosa	β Cru	0350	B0.5 II, B2 V
1.39	Regulus	α Leo	0077	B7 V
1.50	Adhara	ε CMa	0430	B2 Iab:
1.62	Shaula	λ Sco	0700	B2 IV
1.62 (1.98 + 2.97)	Castor	α Gem	0052	Am, A1 V
1.64	Gacrux	γ Cru	0088	M3.5 III
1.64	Bellatrix	γ Ori	0240	B2 III
1.65	Elnath	β Tau	0130	B7 III
1.69	Miaplacidus	β Car	0110	A1 III
1.69 (1.64 - 1.74var)	Alnilam	ε Ori	2,000	B0 Ia
1.72 (1.81 - 1.87var + 4.27)	–	γ Vel	0840	WC8, O7.5e
1.74	Alnair	α Gru	0100	B7 IV
1.77	Alioth	ε UMa	0081	A1 III-IVp kB9
1.77	Alnitak	ζ Ori A	0820	O9.7 Ib, O9 III, B0 II-IV
1.79	Dubhe	α UMa	0120	G9 III, A7.5
1.80	Mirfak	α Per	0590	F5 Ib
1.82	Wezen	δ CMa	1,800	F8 Ia
1.84	Sargas	θ Sco	0270	F0 II
1.85	Kaus Australis	ε Sgr	0140	B9.5 III
1.86	Avior	ε Car	0630	K3 III, B2 Vp
1.86	Alkaid	η UMa	0100	B3 V
1.90 (1.89 - 1.94var)	Menkalinan	β Aur	0100	A1mIV+A1mIV
1.91	Atria	α TrA	0420	K2 IIb-IIIa
1.92	Alhena	γ Gem	0100	A1.5 IV+
1.94	Peacock	α Pav	0180	B2 IV
1.96 (1.99 - 2.39var + 5.57)	–	δ Vel	0080	A1 Va(n), F2-F5
1.98	Mirzam	β CMa	0500	B1 II-III
2.00	Alphard	α Hya	0180	K3 II-III
1.98 (1.86 - 2.13var)	Polaris	α UMi	0430	F8 Ib
2.00	Hamal	α Ari	0066	K1 IIIb
2.08 (2.37 + 3.64)	Algieba	γ Leo	0130	K0 III, G7 IIIb
2.02	Diphda	β Cet	0096	K0 III
2.05	Nunki	σ Sgr	0220	B2.5 V
2.06	Menkent	θ Cen	0061	K0 III
2.05 (2.01 - 2.10var)	Mirach	β And	0200	M0III
2.06	Alpheratz	α And	0097	B8 IV
2.07	Rasalhague	α Oph	0047	A5 V
2.08	Kochab	β UMi	0130	K4 III
2.09	Saiph	κ Ori	0720	B0 Iab:
2.11	Denebola	β Leo	0036	A3 Va
2.12 (2.1 - 3.39var)	Algol	β Per	0093	B8 V
2.15 (2.0 - 2.3var)	–	β Gru	0170	M5 III
2.17	–	γ Cen	0130	A1IV, (A0III/A0III)
2.21	Aspidiske	ι Car	0690	A9 Ib
2.21 (2.14 - 2.30var)	Suhail	λ Vel	0570	K4.5 Ib-II
2.23 (2.21 - 2.32var)	Alphecca	α CrB	0075	A0 V, G5 V
2.23 (2.23 - 2.35var)	Mintaka	δ Ori	0900	B0 III, O9 V
2.23	Sadr	γ Cyg	1,500	F8 Ib
2.23	Eltanin	γ Dra	0150	K5 III
2.24	Schedar	α Cas	0230	K0 IIIa
2.25	Naos	ζ Pup	1,100	O4 If(n)p
2.26	Almach	γ And	0350	K3 IIb, B9.5 V, B9.5 V, A0 V
2.27	Mizar	ζ UMa	0078	A2 Vp, A2 Vp, A1m, A5 V
2.28 (2.25 - 2.31var)	Caph	β Cas	0054	F2 III
2.29	Izar	ε Boo	0202	K0 II-III, A2 V
2.30 (2.29 - 2.34var)	–	α Lup	0550	B1.5 III
2.30 (2.29 - 2.31var)	–	ε Cen	0380	B1III
2.31 (1.6 - 2.32var)	Dschubba	δ Sco	0400	B0.3 IV
2.31	–	ε Sco	0065	K1 III
2.35 (2.30 - 2.41var)	–	η Cen	0310	B1.5Vne
2.37	Merak	β UMa	0079	A1 IVps
2.38	Ankaa	α Phe	0077	K0.5 IIIb
2.39	–	κ Sco	0460	B1.5 III
2.40 (0.7 - 3.0var)	Enif	ε Peg	0670	K2 Ib
2.42 (2.31 - 2.74var)	Scheat	β Peg	0200	M2.5 II-IIIe
2.43	Sabik	η Oph	0049	A1 V, A3 V
2.44	Phecda	γ UMa	0084	A0Ve
2.45	Aludra	η CMa	2,000	B5 Ia
2.46	–	κ Vel	0540	B2 IV
2.47 (1.6 - 3.0var)	–	γ Cas	0610	B0.5 IVpe
2.48	Markab	α Peg	0140	B9 III
2.48	–	ε Cyg	0072	K0 III-IV
2.50	Acrab	β Sco	0404	B1V, B2V

Notes

References

Graham M. Harper, Alexander Brown, and Edward F. Guinan, (April 2008). "A New VLA-Hipparcos Distance to Betelgeuse and its Implications" (PDF). The Astronomical Journal. 135 (4, ). IOP Publishing: 1430–1440. Bibcode:2008AJ....135.1430H. doi:10.1088/0004-6256/135/4/1430. Retrieved 2010-07-10.{{cite journal}}: CS1 maint: extra punctuation (link) CS1 maint: multiple names: authors list (link)
van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.

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