Бележки
Обекти включени в пътеводителя
- Ярки звезди
- деклинация δ2000 > -45°, звездна величина V <= 4.0m ;
- 432 звезди;
- Кратни звезди
- деклинация δ2000 > -45°, звездна величина Va <= 5.0-5.5m, разстояние Δ>=25";
- Кратни звезди: 14 видими с просто око, 67 видими с бинокъл, 74 видими с телескоп;
- Променливи звезди
- деклинация δ2000 > -45°, звездна величина Vmax <= 5.0-5.5m, изменение ΔV>=0.5m;
- Променливи звезди: 13 затъмнителни, 12 цефеиди, 15 дългопериодични, 24 полуправилни, 19 неправилни;
- Звездни купове
- деклинация δ2000 > -45°, звездна величина V < 9.0m;
- Разсеяни звездни купове: 21 видими с просто око, 48 видими с бинокъл, 4 видими с телескоп;
- Сферични звездни купове: 36 видими с бинокъл, 1 видим с телескоп;
- Междузвездно вещество
- деклинация δ2000 > -45°, звездна величина V < 9.0m;
- Йонизирани мъглявини: 2 видими с просто око, 10 видими с бинокъл, 2 видима с телескоп;
- Отражателни мъглявини: 1 видима просто око, 1 видима с бинокъл, 1 видима с телескоп;
- Планетарни мъглявини: 3 видими с бинокъл и 11 видими с телескоп;
- Останки от свръхнова: 2 видими с бинокъл и 1 видима с телескоп;
- Галактики
- деклинация δ2000 > -45°, звездна величина V < 9.0m;
- Галактики: 1 видима с просто око, 20 видими с бинокъл, 39 видими с телескоп;
- Звездни карти
- звездна величина V <= 6.5m;
Съзвездия видими от България
_______________________________________________________________________ Име Брой: Звезди Звезди Други Българско Латинско Съкращение до 6.5V в пътеводителя _______________________________________________________________________ Андромеда Andromeda And 150 9 5 Бик (Телец) Taurus Tau 220 26 4 Близнаци Gemini Gem 120 13 3 Везни Libra Lib 90 7 - Водолей Aquarius Aqr 170 13 5 Воловар Bootes Boo 140 14 - Вълк Lupus Lup 120/70 8 1 Гарван Corvus Crv 30 5 - Голяма мечка Ursa Major UMa 210 22 7 Голямо куче Canus Major CMa 150 16 4 Гущер Lacerta Lac 70 3 1 Гълъб Columba Col 70 6 1 Дева Virgo Vir 170 12 9 Делфин Delphinus Del 40 4 - Длето Caelum Cae 20/18 1 - Дракон Draco Dra 220 19 1 Еднорог Monoceros Mon 140 7 7 Еридан Eridanus Eri 200/180 14 - Жерав Grus Gru Жираф Camelopardalis Cam 160 4 2 Жребче (Малък кон) Equuleus Equ 20 3 - Заек Lepus Lep 70 11 1 Змиеносец Ophiuchus Oph 170 18 10 Змия Serpens Ser 110 10 3 Касиопея Cassiopeia Cas 160 14 9 Кит Cetus Cet 190 14 3 Козирог Capricornus Cap 80 7 1 Колар Auriga Aur 160 12 4 Компас Pyxis Pyx 40 3 - Корабни платна Vela Vel Косите на Вероника Coma Berenices Com 70 5 13 Кърма Puppis Pup 240/200 15 8 Лебед Cygnus Cyg 270 23 8 Лира Lyra Lyr 70 8 2 Ловджийски кучета Canes Venatici CVn 60 4 9 Лъв Leo Leo 120 15 9 Малка лисица Vulpecula Vul 70 2 3 Малка мечка Ursa Minor UMi 40 3 - Малко куче Canis Minor CMi 50 3 - Малък лъв Leo Minor LMi 40 3 - Микроскоп Microscopium Mic 40 2 - Овен Aries Ari 90 5 - Орел Aquila Aql 130 13 2 Орион Orion Ori 200 25 6 Пегас Pegasus Peg 180 10 2 Персей Perseus Per 160 14 7 Пещ Fornax For 60 1 1 Помпа Antlia Ant 40 2 - Рак Cancer Cnc 100 7 2 Риби Pisces Psc 150 9 1 Рис Lynx Lyn 100 5 - Северна корона - Corona Borealis - CrB 40 8 - Секстант Sextans Sex 40 1 1 Скорпион Scorpius Sco 170 23 10 Скулптор Sculptor Scl 50 1 3 Стрела Sagitta Sge 30 4 1 Стрелец Sagittarius Sgr 200 21 17 Триъгълник Triangulum Tri 30 5 1 Феникс Phoenix Phe Херкулес Hercules Her 240 19 3 Хидра Hydra Hya 240 17 4 Центавър Centaurus Cen 280/130 11 1 Цефей Cepheus Cep 160 13 4 Часовник Horologium Hor Чаша Crater Crt 30 3 - Щит Scutum Sct 30 2 3 Ъгломер Norma Nor Южна корона Corona Australis CrA 40 3 1 Южна риба Piscis Austrinus PsA 50 2 - _______________________________________________________________________
Оптични инструменти.
_____________________________________________________________________________
* Инструмент Увеличение Апертура Максимална Зрително Разделителна
входна зв.вел. поле способност
_____________________________________________________________________________
О Просто око 1x 6mm 6 120° 300"
б Оперен бинокъл 3x 20mm 6 15° 100"
б Обикновен бинокъл 6x 30mm 8 7° 50"
Б Астро. бинокъл 12x 50mm 10 4° 25"
т Малък телескоп 60x 75mm 11 50' 5"
Т Телескоп 35x 150mm 13 80' 8"
Т Телескоп 350x 150mm 13 8' 0.8"
_____________________________________________________________________________
Гръцка азбука.
α алфа η ета ν ни τ тау β бета θ тета ξ кси υ ипсилон γ гама ι йота ο омикрон φ фи δ делта κ капа π пи χ хи ε епсилон λ ламбда ρ ро ψ пси ζ дзета μ мю σ сигма ω омега
Спектрална класификация.
Температурни класове.
Класове светимост.
- 0, Ia-, Ia+
- хипергиганти
- Ia, Iab, Ib
- свръхгиганти
- II
- ярки гиганти
- II-III, IIIa, IIIab, IIIb, III-IV
- гиганти
- IV
- субгиганти
- V
- джуджета, главна последователност
- VI
- субджуджета
Особености.
- -
- променлив спектър от/до
- +
- комбиниран спектър
- v
- променлив спектър
- e
- спектър с емисионни линии
- sh
- спектър на обкръжението на звездата
- p
- спектър с особености
- s
- ясен (остър) профил на спектралната линия
- n; nn
- неясен (разлят) профил на спектралната линия; много неясен профил
- CN
- особеност в съдържанието на CN
- w
- слаба линия
- m
- линии на метали
Типове променливи звезди.
Използвана е информация от "General Catalog of Variable Stars (GCVS database, Version 2013 Apr.) Samus N.N., Goranskij V.P., Durlevich O.V., Kazarovets E V., Kireeva N.N., Pastukhova E.N., Zharova A.V. ".
1. eruptive (FU, GCAS, I, IA, IB, IN, INA, INB, INT, IT, IN(YY), IS, ISA,
ISB, RCB, RS, SDOR, UV, UVN, WR),
2. pulsating (ACYG, BCEP, BCEPS, CEP, CEP(B), CW, CWA, CWB, DCEP, DCEPS,
DSCT, DSCTC, GDOR, L, LB, LC, M, PVTEL, RPHS, RR, RR(B), RRAB,
RRC, RV, RVA, RVB, SR, SRA, SRB, SRC, SRD, SXPHE, ZZ, ZZA, ZZB),
3. rotating (ACV, ACVO, BY, ELL, FKCOM, PSR, SXARI),
4. cataclysmic (explosive and novalike) variables (N, NA, NB, NC, NL, NR,
SN, SNI, SNII, UG, UGSS, UGSU, UGZ, ZAND),
5. eclipsing binary systems (E, EA, EB, EW, GS, PN, RS, WD, WR, AR, D, DM,
DS, DW, K, KE, KW, SD),
6. intense variable X-ray sources (X, XB, XF, XI, XJ, XND, XNG, XP, XPR,
XPRM, XM),
7. other symbols (BLLAC, CST, GAL, L:, QSO, S, *, +, :).
8. the new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB)
1. Eruptive Variable Stars
Eruptive variables are stars varying in brightness because of
violent processes and flares occurring in their chromospheres
and coronae. The light changes are usually accompanied by shell
events or mass outflow in the form of stellar winds of variable
intensity and/or by interaction with the surrounding interstellar
medium. This class includes the following types:
GCAS Eruptive irregular variables of the Gamma Cas type. These
are rapidly rotating B III-IVe stars with mass outflow from their
equatorial zones. The formation of equatorial rings or disks is
often accompanied by temporary fading. Light amplitudes may reach
1.5 mag in V.
RCB Variables of the R Coronae Borealis type. These are hydrogen-poor,
carbon- and helium-rich, high-luminosity stars belonging to the
spectral types Bpe-R, which are simultaneously eruptive and
pulsating variables. They show slow nonperiodic fadings by 1-9
mag in V lasting from a month or more to several hundred days.
These changes are superposed on cyclic pulsations with amplitudes
up to several tenths of a magnitude and periods in the range
30-100 days.
RS Eruptive variables of the RS Canum Venaticorum type. This type is
ascribed to close binary systems with spectra showing Ca II H and
K in emission, their components having enhanced chromospheric
activity that causes quasi-periodic light variability. The period
of variation is close to the orbital one, and the variability
amplitude is usually as great as 0.2 mag in V (UX Ari). They are
X-ray sources and rotating variables. RS CVn itself is also an
eclipsing system (see below).
SDOR Variables of the S Doradus type. These are eruptive,
high-luminosity Bpec-Fpec stars showing irregular (sometimes
cyclic) light changes with amplitudes in the range 1-7 mag in V.
They belong to the brightest blue stars of their parent galaxies.
As a rule, these stars are connected with diffuse nebulae and
surrounded by expanding envelopes (P Cyg, Eta Car).
UV Eruptive variables of the UV Ceti type, these are K Ve-M Ve
stars sometimes displaying flare activity with amplitudes from several
tenths of a magnitude up to 6 mag in V. The amplitude is considerably
greater in the ultraviolet spectral region. Maximum light is attained in
several seconds or dozens of seconds after the beginning of a flare; the
star returns to its normal brightness in several minutes or dozens of minutes.
2. Pulsating Variable Stars
Pulsating variables are stars showing periodic expansion and
contraction of their surface layers. The pulsations may be radial
or nonradial. A radially pulsating star remains spherical in
shape, while in the case of nonradial pulsations the star's shape
periodically deviates from a sphere, and even neighboring zones of
its surface may have opposite pulsation phases.
Depending on the period value, on the mass and evolutionary status
of the star, and on the scale of pulsational phenomena, the
following types of pulsating variables may be distinguished:
DCEP These are the classical cepheids, or Delta Cep-type variables. Com-
paratively young objects that have left the main sequence and
evolved into the instability strip of the Hertzsprung-Russell
(H-R) diagram, they obey the well-known Cepheid period-luminosity
relation and belong to the young disk population. DCEP stars are
present in open clusters. They display a certain relation between
the shapes of their light curves and their periods.
DCEPS These are Delta Cep variables having light amplitudes <0.5 mag in
V (<0.7 mag in B) and almost symmetrical light curves (M-m
approx. 0.4 - 0.5 periods); as a rule, their periods do not exceed
7 days. They are probably first-overtone pulsators and/or are in
the first transition across the instability strip after leaving
the main sequence (SU Cas).
LB Slow irregular variables of late spectral types (K, M, C, S); as a
rule, they are giants (CO Cyg). This type is also ascribed, in
the GCVS, to slow red irregular variables in the case of unknown
spectral types and luminosities.
LC Irregular variable supergiants of late spectral types having amplitudes
of about 1 mag in V (TZ Cas).
M Mira (Omicron) Ceti-type variables. These are long-period variable
giants with characteristic late-type emission spectra (Me, Ce, Se) and
light amplitudes from 2.5 to 11 mag in V. Their periodicity is
well pronounced, and the periods lie in the range between 80 and
1000 days. Infrared amplitudes are usually less than in the
visible and may be <2.5 mag. For example, in the K band they
usually do not exceed 0.9 mag. If the amplitudes exceed 1 - 1.5
mag , but it is not certain that the true light amplitude exceeds 2.5
mag, the symbol "M" is followed by a colon, or the star is
attributed to the semiregular class with a colon following the
symbol for that type (SR).
RVA RV Tauri variables that do not vary in mean magnitude (AC Her);
RVB RV Tauri variables that periodically (with periods from 600 to
1500 days and amplitudes up to 2 mag in V) vary in mean
magnitude (DF Cyg, RV Tau).
SR Semiregular variables, which are giants or supergiants of intermediate
and late spectral types showing noticeable periodicity in their
light changes, accompanied or sometimes interrupted by various
irregularities. Periods lie in the range from 20 to >2000 days,
while the shapes of the light curves are rather different and
variable, and the amplitudes may be from several hundredths to
several magnitudes (usually 1-2 mag in V).
SRA Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying
persistent periodicity and usually small (<2.5 mag in V) light
amplitudes (Z Aqr). Amplitudes and light-curve shapes generally
vary and periods are in the range of 35-1200 days. Many of these
stars differ from Miras only by showing smaller light amplitudes;
SRB Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly
defined periodicity (mean cycles in the range of 20 to 2300 days)
or with alternating intervals of periodic and slow irregular changes,
and even with light constancy intervals (RR CrB, AF Cyg). Every star
of this type may usually be assigned a certain mean period
(cycle), which is the value given in the Catalogue. In a number
of cases, the simultaneous presence of two or more periods of
light variation is observed;
SRC Semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with
amplitudes of about 1 mag and periods of light variation from 30 days to
several thousand days;
SRD Semiregular variable giants and supergiants of F, G, or K spectral
types, sometimes with emission lines in their spectra. Amplitudes
of light variation are in the range from 0.1 to 4 mag, and the range of
periods is from 30 to 1100 days (SX Her, SV UMa).
3. Rotating Variable Stars
Variable stars with nonuniform surface brightness and/or
ellipsoidal shapes, whose variability is caused by axial rotation
with respect to the observer. The nonuniformity of surface
brightness distributions may be caused by the presence of spots or
by some thermal or chemical inhomogeneity of the atmosphere caused
by a magnetic field whose axis is not coincident with the rotation
axis. These stars are subdivided into the following types:
ACV Alpha2 Canum Venaticorum variables. These are main-sequence stars
with spectral types B8p-A7p and displaying strong magnetic fields.
Spectra show abnormally strong lines of Si, Sr, Cr, and rare
earths whose intensities vary with rotation. They exhibit magnetic
field and brightness changes (periods of 0.5-160 days or more). The
amplitudes of the brightness changes are usually withine 0.01-0.1 mag
in V.
4. Cataclysmic (Explosive and Novalike) Variables
These are variable stars showing outbursts caused by thermonuclear
burst processes in their surface layers (novae) or deep in their
interiors (supernovae). We use the term "novalike" for
variables that show novalike outbursts caused by rapid energy
release in the surrounding space (UG-type stars - see
below) and also for objects not displaying outbursts but
resembling explosive variables at minimum light by their spectral
(or other) characteristics. The majority of explosive and
novalike variables are close binary systems, their components
having strong mutual influence on the evolution of each star. It
is often observed that the hot dwarf component of the system is
surrounded by an accretion disk formed by matter lost by the
other, cooler, and more extended component. This category is
subdivided into the following types:
NR Recurrent novae, which differ from typical novae by the fact that two
or more outbursts (instead of a single one) separated by 10-80
years have been observed (T CrB).
ZAND Symbiotic variables of the Z Andromedae type. They are close
binaries consisting of a hot star, a star of late type, and an
extended envelope excited by the hot star's radiation. The
combined brightness displays irregular variations with amplitudes
up to 4 mag in V. A very inhomogeneous group of objects.
5. Close Binary Eclipsing Systems
We adopt a triple system of classifying eclipsing binary systems:
according to the shape of the combined light curve, as well as to
physical and evolutionary characteristics of their components.
The classification based on light curves is simple, traditional,
and suits the observers; the second and third classification
methods take into account positions of the binary-system
components in the (MV ,B-V) diagram and the degree of inner Roche
lobe filling. Estimates are made by applying the simple criteria
proposed by Svechnikov and Istomin (1979). The symbols for the
types of eclipsing binary systems that we use are given below.
a) Classification based on the shape of the light curve
EA Algol (Beta Persei)-type eclipsing systems. Binaries with spherical
or slightly ellipsoidal components. It is possible to specify, for
their light curves, the moments of the beginning and end of the
eclipses. Between eclipses the light remains almost constant or
varies insignificantly because of reflection effects, slight
ellipsoidality of components, or physical variations. Secondary
minima may be absent. An extremely wide range of periods is
observed, from 0.2 to >= 10000 days. Light amplitudes are also
quite different and may reach several magnitudes.
EB Beta Lyrae-type eclipsing systems. These are eclipsing systems having
ellipsoidal components and light curves for which it is impossible
to specify the exact times of onset and end of eclipses because of
a continuous change of a system's apparent combined brightness
between eclipses; secondary minimum is observed in all cases, its
depth usually being considerably smaller than that of the primary
minimum; periods are mainly longer than 1 day. The components
generally belong to early spectral types (B-A). Light amplitudes
are usually <2 mag in V.
EW W Ursae Majoris-type eclipsing variables. These are eclipsers with
periods shorter than 1 days, consisting of ellipsoidal components
almost in contact and having light curves for which it is
impossible to specify the exact times of onset and end of
eclipses. The depths of the primary and secondary minima are
almost equal or differ insignificantly. Light amplitudes are
usually <0.8 mag in V. The components generally belong to
spectral types F-G and later.
b) Classification according to the components' physical
characteristics
GS Systems with one or both giant and supergiant components; one of the
components may be a main sequence star.
c) Classification based on the degree of filling of inner Roche
lobes
DM Detached main-sequence systems. Both components are main-sequence
stars and do not fill their inner Roche lobes.
KE Contact systems of early (O-A) spectral type, both components being
close in size to their inner critical surfaces.
SD Semidetached systems in which the surface of the less massive com-
ponent is close to its inner Roche lobe.
The combination of the above three classification systems for
eclipsers results in the assignment of multiple classifications
for object types. These are separated by a solidus ("/") in the
data field. Examples are: E/DM, EA/DS/RS, EB/WR, EW/KW, etc.
6. Optically Variable Close Binary Sources of Strong, Variable
X-ray Radiation (X-ray Sources)
XP X-ray pulsar systems. The primary component is usually an ellipsoidal
early-type supergiant. The reflection effect is very small and
light variability is mainly caused by the ellipsoidal primary
component's rotation. Periods of light changes are between 1 and
10 days; the period of the pulsar in the system is from 1 s to 100
min. Light amplitudes usually do not exceed several tenths of a
magnitude (Vela X-1 = GP Vel);
Използвана литература.
2000,A&AS,143,9 , "The SIMBAD astronomical database", Wenger et al.
Washington Double Star Catalog maintained at the U.S. Naval Observatory
G and K giant stars stellar parameters (Reffert+, 2015)
Fundamental parameters of stars (Allende Prieto+, 1999)
Андрейчин Разум, Томалевски Георги, Нашето звездно небе, "Народна просвета" София 1960
Karkoschka E., The Observer's Sky Atlas, "Springer" 2007
Ридпат Ян, Звезды и планеты, "АСТ и Астрель" Москва 2004