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38-564: M48 or M-48 may refer to: Messier 48 , an open star cluster in the constellation Hydra 48th known Mersenne prime M48 Patton , an American tank MIM-72A/M48 Chaparral , an American self-propelled surface-to-air missile system M-48 (Michigan highway) , a state highway in Michigan M48 motorway , a motorway in Great Britain between England and Wales M48 (Cape Town) ,

76-684: A Metropolitan Route in Cape Town, South Africa M48 (Johannesburg) , a Metropolitan Route in Johannesburg, South Africa M48 Mauser , a Yugoslavian version of the Mauser K98 rifle 76 mm mountain gun M48 , a Yugoslavian mountain gun Zastava M48 , a post World War II Yugoslavian version of the German Karabiner 98k [REDACTED] Topics referred to by the same term This disambiguation page lists articles associated with

114-547: A few elements or isotopes, so a star or gas sample with certain   [ ? F e ] ⋆   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {?}}{\mathsf {Fe}}}{\bigr ]}_{\star }\ } values may well be indicative of an associated, studied nuclear process. Astronomers can estimate metallicities through measured and calibrated systems that correlate photometric measurements and spectroscopic measurements (see also Spectrophotometry ). For example,

152-522: A giant planet. Measurements have demonstrated the connection between a star's metallicity and gas giant planets, like Jupiter and Saturn . The more metals in a star and thus its planetary system and protoplanetary disk , the more likely the system may have gas giant planets. Current models show that the metallicity along with the correct planetary system temperature and distance from the star are key to planet and planetesimal formation. For two stars that have equal age and mass but different metallicity,

190-404: A mass of 2,366  M ☉ . The general structure of the cluster is fragmented and lumpy, which may be due to interactions with the galactic disk . The cluster is now subdivided into three groups, each of which has its own collective proper motion . Metallicity#Chemical abundance ratios In 1802, William Hyde Wollaston noted the appearance of a number of dark features in

228-407: A star will die: Outside the pair-instability window , lower metallicity stars will collapse directly to a black hole, while higher metallicity stars undergo a type Ib/c supernova and may leave a neutron star . A star's metallicity measurement is one parameter that helps determine whether a star may have a giant planet , as there is a direct correlation between metallicity and the presence of

266-418: Is an open cluster of stars in the equatorial constellation of Hydra . It sits near Hydra's westernmost limit with Monoceros , about 18° 34′ to the east and slightly south of Hydra's brightest star, Alphard . This grouping was discovered by Charles Messier in 1771, but there is no cluster precisely where Messier indicated; he made an error, as he did with M47. The value that he gave for

304-473: Is considered to be relatively constant in the Universe, or the iron content of the star, which has an abundance that is generally linearly increasing in time in the Universe. Hence, iron can be used as a chronological indicator of nucleosynthesis. Iron is relatively easy to measure with spectral observations in the star's spectrum given the large number of iron lines in the star's spectra (even though oxygen

342-408: Is known as photoionization . The free electrons can strike other atoms nearby, exciting bound metallic electrons into a metastable state , which eventually decay back into a ground state, emitting photons with energies that correspond to forbidden lines . Through these transitions, astronomers have developed several observational methods to estimate metal abundances in H regions, where the stronger

380-1112: Is the most abundant heavy element – see metallicities in H regions below). The abundance ratio is the common logarithm of the ratio of a star's iron abundance compared to that of the Sun and is calculated thus: [ F e H ]   =   log 10 ⁡ ( N F e N H ) ⋆ −   log 10 ⁡ ( N F e N H ) ⊙   , {\displaystyle \left[{\frac {\mathsf {Fe}}{\mathsf {H}}}\right]~=~\log _{10}{\left({\frac {N_{\mathsf {Fe}}}{N_{\mathsf {H}}}}\right)_{\star }}-~\log _{10}{\left({\frac {N_{\mathsf {Fe}}}{N_{\mathsf {H}}}}\right)_{\odot }}\ ,} where   N F e   {\displaystyle \ N_{\mathsf {Fe}}\ } and   N H   {\displaystyle \ N_{\mathsf {H}}\ } are

418-1505: Is the sum of the fluxes from oxygen emission lines measured at the rest frame λ = (3727, 4959 and 5007) Å wavelengths, divided by the flux from the Balmer series H β emission line at the rest frame λ = 4861 Å wavelength. This ratio is well defined through models and observational studies, but caution should be taken, as the ratio is often degenerate, providing both a low and high metallicity solution, which can be broken with additional line measurements. Similarly, other strong forbidden line ratios can be used, e.g. for sulfur, where S 23 =   [   S I I ] 6716   Å + 6731   Å + [   S I I I ] 9069   Å + 9532   Å   [   H β ] 4861   Å   . {\displaystyle S_{23}={\frac {\ \left[\ {\mathsf {S}}^{\mathsf {II}}\right]_{6716~\mathrm {\AA} +6731~\mathrm {\AA} }+\left[\ {\mathsf {S}}^{\mathsf {III}}\right]_{9069~\mathrm {\AA} +9532~\mathrm {\AA} }\ }{{\Bigl [}\ {\mathsf {H}}_{\mathsf {\beta }}{\Bigr ]}_{4861~\mathrm {\AA} }}}~.} Metal abundances within H regions are typically less than 1%, with

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456-483: Is visible to the naked eye under good atmospheric conditions. The brightest member is the star HIP 40348 at visual magnitude 8.3. The cluster is located some 2,500 light-years from the Sun. The age estimated from isochrones is 400 ± 100  Myr, while gyrochronology age estimate is 450 ± 50  Myr – in good agreement. This makes it intermediate in age between the Pleiades , at around 100 Myr, and

494-518: The Hyades , at about 650 Myr. The metallicity of the cluster, based on the abundance of iron (Fe), is [Fe/H] = −0.063 ± 0.007  dex , where −1 would be ten times lower than in the Sun. It is more metal-poor than the Pleiades, Hyades, and Praesepe clusters. The cluster has a tidal radius of 63.3 ± 7.8 ly (19.4 ± 2.4 pc) with at least 438 members and

532-496: The Hyades cluster . Unfortunately, δ (U−B) is sensitive to both metallicity and temperature : If two stars are equally metal-rich, but one is cooler than the other, they will likely have different δ (U−B) values (see also Blanketing effect ). To help mitigate this degeneracy, a star's B−V  color index can be used as an indicator for temperature. Furthermore, the UV ;excess and B−V index can be corrected to relate

570-522: The Johnson UVB filters can be used to detect an ultraviolet (UV) excess in stars, where a smaller UV excess indicates a larger presence of metals that absorb the UV radiation, thereby making the star appear "redder". The UV excess, δ (U−B), is defined as the difference between a star's U and B band magnitudes , compared to the difference between U and B band magnitudes of metal-rich stars in

608-490: The Sun . Stellar composition is often simply defined by the parameters X , Y , and Z . Here X represents the mass fraction of hydrogen , Y is the mass fraction of helium , and Z is the mass fraction of all the remaining chemical elements. Thus X + Y + Z = 1 {\displaystyle X+Y+Z=1} In most stars , nebulae , H regions , and other astronomical sources, hydrogen and helium are

646-1530: The infrared spectrum. Oxygen has some of the stronger, more abundant lines in H regions, making it a main target for metallicity estimates within these objects. To calculate metal abundances in H regions using oxygen flux measurements, astronomers often use the R 23 method, in which R 23 =   [   O I I ] 3727   Å + [   O I I I ] 4959   Å + 5007   Å   [   H β ] 4861   Å   , {\displaystyle R_{23}={\frac {\ \left[\ {\mathsf {O}}^{\mathsf {II}}\right]_{3727~\mathrm {\AA} }+\left[\ {\mathsf {O}}^{\mathsf {III}}\right]_{4959~\mathrm {\AA} +5007~\mathrm {\AA} }\ }{{\Bigl [}\ {\mathsf {H}}_{\mathsf {\beta }}{\Bigr ]}_{4861~\mathrm {\AA} }}}\ ,} where   [   O I I ] 3727   Å + [   O I I I ] 4959   Å + 5007   Å   {\displaystyle \ \left[\ {\mathsf {O}}^{\mathsf {II}}\right]_{3727~\mathrm {\AA} }+\left[\ {\mathsf {O}}^{\mathsf {III}}\right]_{4959~\mathrm {\AA} +5007~\mathrm {\AA} }\ }

684-438: The right ascension matches, however, his declination is off by five degrees. Credit for discovery is sometimes given instead to Caroline Herschel in 1783. Her nephew John Herschel described it as, "a superb cluster which fills the whole field; stars of 9th and 10th to the 13th magnitude – and none below, but the whole ground of the sky on which it stands is singularly dotted over with infinitely minute points". M48

722-650: The δ (U−B) value to iron abundances. Other photometric systems that can be used to determine metallicities of certain astrophysical objects include the Strӧmgren system, the Geneva system, the Washington system, and the DDO system. At a given mass and age, a metal-poor star will be slightly warmer. Population II stars ' metallicities are roughly ⁠ 1 / 1000 ⁠ to ⁠ 1 / 10 ⁠ of

760-403: The "first-born" stars created in the Universe. Astronomers use several different methods to describe and approximate metal abundances, depending on the available tools and the object of interest. Some methods include determining the fraction of mass that is attributed to gas versus metals, or measuring the ratios of the number of atoms of two different elements as compared to the ratios found in

798-545: The Sun (10 ); conversely, those with a   [ F e H ] ⋆   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {Fe}}{\mathsf {H}}}{\bigr ]}_{\star }\ } value of −1 have ⁠ 1 / 10 ⁠ , while those with a   [ F e H ] ⋆   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {Fe}}{\mathsf {H}}}{\bigr ]}_{\star }\ } value of 0 have

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836-406: The Sun have a positive common logarithm , whereas those more dominated by hydrogen have a corresponding negative value. For example, stars with a   [ F e H ] ⋆   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {Fe}}{\mathsf {H}}}{\bigr ]}_{\star }\ } value of +1 have 10 times the metallicity of

874-529: The Sun's (   [ F e H ]   = − 3.0   . . .   − 1.0   )   , {\displaystyle \left(\ {\bigl [}{\tfrac {\mathsf {Fe}}{\mathsf {H}}}{\bigr ]}\ ={-3.0}\ ...\ {-1.0}\ \right)\ ,} but the group appears cooler than population I overall, as heavy population II stars have long since died. Above 40  solar masses , metallicity influences how

912-535: The forbidden lines in spectroscopic observations, the higher the metallicity. These methods are dependent on one or more of the following: the variety of asymmetrical densities inside H regions, the varied temperatures of the embedded stars, and/or the electron density within the ionized region. Theoretically, to determine the total abundance of a single element in an H region, all transition lines should be observed and summed. However, this can be observationally difficult due to variation in line strength. Some of

950-627: The hydrogen it contains. Similarly, the helium mass fraction is denoted as   Y ≡ m H e M   . {\displaystyle \ Y\equiv {\tfrac {m_{\mathsf {He}}}{M}}~.} The remainder of the elements are collectively referred to as "metals", and the mass fraction of metals is calculated as Z = ∑ e > H e m e M = 1 − X − Y   . {\displaystyle Z=\sum _{e>{\mathsf {He}}}{\tfrac {m_{e}}{M}}=1-X-Y~.} For

988-600: The less metallic star is bluer . Among stars of the same color, less metallic stars emit more ultraviolet radiation. The Sun, with eight planets and nine consensus dwarf planets , is used as the reference, with a   [ F e H ]   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {Fe}}{\mathsf {H}}}{\bigr ]}\ } of 0.00. Young, massive and hot stars (typically of spectral types O and B ) in H regions emit UV photons that ionize ground-state hydrogen atoms, knocking electrons free; this process

1026-435: The metals into the surrounding environment, enriching the interstellar medium and providing recycling materials for the birth of new stars . It follows that older generations of stars, which formed in the metal-poor early Universe , generally have lower metallicities than those of younger generations, which formed in a more metal-rich Universe. Observed changes in the chemical abundances of different types of stars, based on

1064-431: The most common forbidden lines used to determine metal abundances in H regions are from oxygen (e.g. [O ] λ = (3727, 7318, 7324) Å, and [O ] λ = (4363, 4959, 5007) Å), nitrogen (e.g. [N ] λ = (5755, 6548, 6584) Å), and sulfur (e.g. [S ] λ = (6717, 6731) Å and [S ] λ = (6312, 9069, 9531) Å) in the optical spectrum, and the [O ] λ = (52, 88) μm and [N ] λ = 57 μm lines in

1102-403: The notation   [ O F e ]   {\displaystyle \ {\bigl [}{\tfrac {\mathsf {O}}{\mathsf {Fe}}}{\bigr ]}\ } represents the difference in the logarithm of the star's oxygen abundance versus its iron content compared to that of the Sun. In general, a given stellar nucleosynthetic process alters the proportions of only

1140-407: The number of iron and hydrogen atoms per unit of volume respectively, ⊙ {\displaystyle \odot } is the standard symbol for the Sun, and ⋆ {\displaystyle \star } for a star (often omitted below). The unit often used for metallicity is the dex , contraction of "decimal exponent". By this formulation, stars with a higher metallicity than

1178-450: The same metallicity as the Sun, and so on. Young population I stars have significantly higher iron-to-hydrogen ratios than older population II stars. Primordial population III stars are estimated to have metallicity less than −6, a millionth of the abundance of iron in the Sun. The same notation is used to express variations in abundances between other individual elements as compared to solar proportions. For example,

M48 - Misplaced Pages Continue

1216-550: The same title formed as a letter–number combination. If an internal link led you here, you may wish to change the link to point directly to the intended article. Retrieved from " https://en.wikipedia.org/w/index.php?title=M48&oldid=1101216794 " Category : Letter–number combination disambiguation pages Hidden categories: Short description is different from Wikidata All article disambiguation pages All disambiguation pages Messier 48 Messier 48 or M48 , also known as NGC 2548 ,

1254-489: The solar spectrum. In 1814, Joseph von Fraunhofer independently rediscovered the lines and began to systematically study and measure their wavelengths , and they are now called Fraunhofer lines . He mapped over 570 lines, designating the most prominent with the letters A through K and weaker lines with other letters. About 45 years later, Gustav Kirchhoff and Robert Bunsen noticed that several Fraunhofer lines coincide with characteristic emission lines identifies in

1292-443: The spectra of heated chemical elements. They inferred that dark lines in the solar spectrum are caused by absorption by chemical elements in the solar atmosphere. Their observations were in the visible range where the strongest lines come from metals such as sodium, potassium, and iron. In the early work on the chemical composition of the sun the only elements that were detected in spectra were hydrogen and various metals, with

1330-448: The spectral peculiarities that were later attributed to metallicity, led astronomer Walter Baade in 1944 to propose the existence of two different populations of stars . These became commonly known as population I (metal-rich) and population II (metal-poor) stars. A third, earliest stellar population was hypothesized in 1978, known as population III stars. These "extremely metal-poor" (XMP) stars are theorized to have been

1368-445: The surface of the Sun ( symbol ⊙ {\displaystyle \odot } ), these parameters are measured to have the following values: Due to the effects of stellar evolution , neither the initial composition nor the present day bulk composition of the Sun is the same as its present-day surface composition. The overall stellar metallicity is conventionally defined using the total hydrogen content, since its abundance

1406-448: The term metallic frequently used when describing them. In contemporary usage in astronomy all the extra elements beyond just hydrogen and helium are termed metallic. The presence of heavier elements results from stellar nucleosynthesis, where the majority of elements heavier than hydrogen and helium in the Universe ( metals , hereafter) are formed in the cores of stars as they evolve . Over time, stellar winds and supernovae deposit

1444-406: The two dominant elements. The hydrogen mass fraction is generally expressed as   X ≡ m H M   , {\displaystyle \ X\equiv {\tfrac {m_{\mathsf {H}}}{M}}\ ,} where M is the total mass of the system, and   m H   {\displaystyle \ m_{\mathsf {H}}\ } is the mass of

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