The Young Age Of The Milky Way Galaxy
|
Hyperlink |
Dating
Method |
Age/Years |
|
AGB Stars |
900,000 |
|
|
https://www.aanda.org/articles/aa/pdf/2019/06/aa35366-19.pdf |
AGB Stars |
1,000,000 |
|
https://www.aanda.org/articles/aa/pdf/2015/07/aa24609-14.pdf |
AGB Stars |
16,000 |
|
https://www.aanda.org/articles/aa/pdf/2022/03/aa42648-21.pdf |
AGB Stars |
60,000 |
|
AGB Stars |
100,000 |
|
|
AGB Stars |
100,000 |
|
|
https://www.aanda.org/articles/aa/pdf/2021/06/aa40072-20.pdf |
Blue Stragglers |
3,000,000 |
|
Carbon Stars |
100,000 |
|
|
Carbon Stars |
100,000 |
|
|
Carbon Stars |
75,000 |
|
|
https://www.aanda.org/articles/aa/pdf/2010/01/aa12084-09.pdf |
Carbon Stars |
500,000 |
|
https://iopscience.iop.org/article/10.3847/1538-3881/ad12bf/pdf |
Dust Shells |
5,000 |
|
Dust Shells |
6,000 |
|
|
https://iopscience.iop.org/article/10.1088/0067-0049/212/1/6 |
Magnetar Spin |
1,700,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
283,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
645,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
509,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
1,217,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
18,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
44,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
7,000 |
|
https://doi.org/10.1093/mnras/stz1391 |
Magnetar Spin |
4,000 |
|
Red Super Giants |
1,000,000 |
|
|
Red Super Giants |
200,000 |
|
|
https://www.aanda.org/articles/aa/pdf/2023/08/aa44770-22.pdf |
Red Super Giants |
700,000 |
|
https://www.aanda.org/articles/aa/pdf/2017/12/aa31590-17.pdf |
Wolf-Rayet Stars |
1,200,000 |
|
https://iopscience.iop.org/article/10.3847/1538-4357/833/2/133/pdf |
Wolf-Rayet Stars |
6,000,000 |
|
https://ui.adsabs.harvard.edu/scan/manifest/2000A%26A...360..227N?art=true |
Wolf-Rayet Stars |
700,000 |
https://www.creationismonline.com/YEC/Young_Galaxy.htm
https://www.creationismonline.com/YEC/Young_Galaxy.xlsm
Introduction
The Milky
Way or Milky Way Galaxy[c], or simply the Galaxy,[28] is the galaxy that includes the Solar System, with the name describing the galaxy's appearance from Earth: a hazy band of light seen in the night sky formed from stars in other
arms of the galaxy, which are so far away that they cannot be individually
distinguished by the naked eye.
Evolutionists believe Globular clusters are among the oldest objects in the Milky Way, thereby setting a lower limit on the age of the Milky Way. The ages of individual stars in the Milky Way can be estimated by measuring the abundance of long-lived radioactive elements such as thorium-232 and uranium-238, then comparing the results to estimates of their original abundance, a technique called nuclear-cosmos chronology. These yield values of about 12.5 ± 3 billion years for CS 31082-001[272] and 13.8 ± 4 billion years for BD +17° 3248.[273] An in depth study shows these methods to be unreliable.
Stellar Age Chronometers
https://www.creationismonline.com/YEC/StellarAges.htm
https://www.creationismonline.com/YEC/ICR.pdf
https://www.creationismonline.com/YEC/Radio_Dating.xlsm
AGB Stars
|
AGB stars, Mass range 0.5 to 8 Solar
Masses |
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (about 0.5 to 8 solar masses) late in their lives.
These stars are ejecting matter at a high rate and thus have a very short life.
1,460 dates less than 1 million years old.
https://www.aanda.org/articles/aa/pdf/2019/06/aa35366-19.pdf
Astronomy & Astrophysics, 626, A100 (2019)
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/626/A100
If the starting mass is 0.5 solar masses the average age is 450,000 years.
“These colors, especially (Ks− [D])0, enable estimation of the mass-loss rates (M.) of the sources in the bulge fields which range from 10−7 to 10−4 M yr−1. Taking into consideration the completeness of the mass-loss rate bins, we find that the contribution to the integrated mass-loss is probably dominated by mass-loss rates larger than 3 × 10−7 M yr−1 and is about 1.96 × 10−4 M yr−1 deg−2 in the ‘intermediate’ and ‘outer’ bulge fields of sources with mass-loss rates, M. > 3×10−7 M yr−1.”
Minimum ages assume a mass of 0.5 Solar Masses.
|
|
Min Ages |
Max Ages |
|
|
Years |
Years |
|
Average |
455,533 |
9,110,666 |
|
Maximum |
1,562,500 |
31,250,000 |
|
Minimum |
9,615 |
192,308 |
|
No. Dates |
1,460 |
1,460 |
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/MNRAS/381/1219
https://doi.org/10.1111/j.1365-2966.2007.12320.x
MNRAS, 381, 1219–1234 (2007)
.
“Extremely reddened asymptotic giant branch stars (AGB) lose mass at high rates of >10−5 M yr−1 . This is the very last stage of AGB evolution, in which stars in the mass range ∼2.0−4.0 M (for solar metallicity) should have been converted to C stars already. The extremely reddened AGB stars in the Galactic bulge are however predominantly O-rich, implying that they might be either low-mass stars or stars at the upper end of the AGB mass range.”
|
|
Min Ages |
Max Ages |
|
|
Years |
Years |
|
Average |
16,694 |
333,890 |
|
Maximum |
50,000 |
1,000,000 |
|
Minimum |
1,238 |
24,752 |
|
No. Dates |
34 |
34 |
https://www.aanda.org/articles/aa/pdf/2015/07/aa24609-14.pdf
Astronomy & Astrophysics, 579, A76(2015)
“Variability is a key property of stars on the asymptotic giant branch (AGB). Their pulsation period is related to the luminosity
and mass-loss rate (MLR) of the star.”
|
|
Min Ages |
Max Ages |
|
|
Years |
Years |
|
Average |
127,922 |
2,558,440 |
|
Maximum |
7,082,153 |
141,643,059 |
|
Minimum |
111 |
2,217 |
|
No. Dates |
121 |
121 |
|
|
Min Ages |
Max Ages |
|
|
Years |
Years |
|
Average |
60,191 |
1,203,823 |
|
Maximum |
287,356 |
5,747,126 |
|
Minimum |
1,634 |
32,680 |
|
No. Dates |
200 |
200 |
https://www.aanda.org/articles/aa/pdf/2022/03/aa42648-21.pdf
Astronomy & Astrophysics, 659, id.A145
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/A%2bA/659/A145/
“Super-AGB stars also reach very high mass-loss rates, in excess of 10−4M⊙yr−1. The mass loss of RSGs appears to be subject to different modes, with rates well below, around, and well above the nuclear burning timescale. The timescale for the dominant mass loss phase is ∼0.6–2 ×105yr, shorter than the thermal-pulsing AGB or RSG phases.”
|
log(M⊙/Year ) |
Years/Solar Mass |
Min Age |
Max Age |
|
-2.79 |
617 |
308 |
4,933 |
|
-3.37 |
2,344 |
1,172 |
18,754 |
|
-3.56 |
3,631 |
1,815 |
29,046 |
|
-3.55 |
3,548 |
1,774 |
28,385 |
|
-3.75 |
5,623 |
2,812 |
44,987 |
|
-3.65 |
4,467 |
2,233 |
35,735 |
|
-3.66 |
4,571 |
2,285 |
36,567 |
|
-3.8 |
6,310 |
3,155 |
50,477 |
|
-4.6 |
39,811 |
19,905 |
318,486 |
|
-4.09 |
12,303 |
6,151 |
98,422 |
|
-3.55 |
3,548 |
1,774 |
28,385 |
|
-4.04 |
10,965 |
5,482 |
87,718 |
|
-4.03 |
10,715 |
5,358 |
85,722 |
|
-3.46 |
2,884 |
1,442 |
23,072 |
|
-4.09 |
12,303 |
6,151 |
98,422 |
|
Mass |
log(M⊙/Year ) |
Years/Solar Mass |
Life Span |
|
3.6 |
-5.27 |
186,209 |
12,176 |
|
3.4 |
-5.32 |
208,930 |
13,676 |
|
3.2 |
-5.4 |
251,189 |
16,446 |
|
3.5 |
-5.28 |
190,546 |
12,477 |
|
3.3 |
-5.3 |
199,526 |
13,070 |
|
3.3 |
-5.35 |
223,872 |
14,665 |
|
3.6 |
-4.94 |
87,096 |
5,716 |
|
Mass |
log(M⊙/Year ) |
Years/Solar Mass |
Life Span |
|
21.1 |
-3.15 |
1,413 |
29,805 |
|
11 |
-3.92 |
8,318 |
91,494 |
|
3.1 |
-5.46 |
288,403 |
894,050 |
|
3.2 |
-5.46 |
288,403 |
922,890 |
|
16.6 |
-4.27 |
18,621 |
309,106 |
|
8.9 |
-4.31 |
20,417 |
181,715 |
|
3.5 |
-5.33 |
213,796 |
748,287 |
|
8.3 |
-3.9 |
7,943 |
65,929 |
https://arxiv.org/pdf/2607.19989
MNRAS
|
AGB |
Annual Loss |
Model One |
Model One |
Annual Loss |
Model Two |
Model Two |
|
STAR |
Sun = 1 |
Min Ages |
Max Ages |
Sun = 1 |
Min Ages |
Max Ages |
|
IRAS-18052 |
2.20E-06 |
227,273 |
3,636,364 |
1.10E-04 |
4,545 |
72,727 |
|
IRAS-18092 |
9.30E-07 |
537,634 |
8,602,151 |
1.10E-04 |
4,545 |
72,727 |
|
IRAS-18100 |
1.50E-06 |
333,333 |
5,333,333 |
2.10E-04 |
2,381 |
38,095 |
|
OH-16.1 |
3.50E-06 |
142,857 |
2,285,714 |
2.90E-04 |
1,724 |
27,586 |
|
IRAS-18257 |
1.40E-06 |
357,143 |
5,714,286 |
1.50E-04 |
3,333 |
53,333 |
|
OH-21.5 |
2.80E-06 |
178,571 |
2,857,143 |
2.60E-04 |
1,923 |
30,769 |
|
IRAS-18327 |
1.20E-06 |
416,667 |
6,666,667 |
1.20E-04 |
4,167 |
66,667 |
|
OH-26.5 |
2.30E-06 |
217,391 |
3,478,261 |
2.60E-04 |
1,923 |
30,769 |
|
IRAS-18361 |
1.40E-06 |
357,143 |
5,714,286 |
1.70E-04 |
2,941 |
47,059 |
|
OH-30.7 |
2.30E-06 |
217,391 |
3,478,261 |
2.60E-04 |
1,923 |
30,769 |
|
OH-30.1 |
2.20E-06 |
227,273 |
3,636,364 |
2.20E-04 |
2,273 |
36,364 |
|
IRAS-18488 |
4.10E-06 |
121,951 |
1,951,220 |
3.60E-04 |
1,389 |
22,222 |
|
OH-32.8 |
2.80E-06 |
178,571 |
2,857,143 |
3.10E-04 |
1,613 |
25,806 |
|
IRAS-18588 |
1.40E-06 |
357,143 |
5,714,286 |
1.30E-04 |
3,846 |
61,538 |
|
OH-39.9 |
1.10E-06 |
454,545 |
7,272,727 |
1.60E-04 |
3,125 |
50,000 |
|
IRAS-19067 |
2.60E-06 |
192,308 |
3,076,923 |
2.70E-04 |
1,852 |
29,630 |
|
IRAS-22177 |
1.20E-06 |
416,667 |
6,666,667 |
1.30E-04 |
3,846 |
61,538 |
|
AFGL-5379 |
2.00E-06 |
250,000 |
4,000,000 |
2.00E-04 |
2,500 |
40,000 |
|
OH-13.1 |
1.80E-06 |
277,778 |
4,444,444 |
2.40E-04 |
2,083 |
33,333 |
|
IRAS-18310 |
1.80E-06 |
277,778 |
4,444,444 |
2.40E-04 |
2,083 |
33,333 |
|
OH-51.8 |
1.70E-06 |
294,118 |
4,705,882 |
1.80E-04 |
2,778 |
44,444 |
|
OH-65.7 |
1.80E-06 |
277,778 |
4,444,444 |
3.20E-04 |
1,563 |
25,000 |
|
OH-75.3 |
1.80E-06 |
277,778 |
4,444,444 |
3.00E-04 |
1,667 |
26,667 |
https://www.aanda.org/articles/aa/pdf/2006/18/aa4569-05.pdf
Astronomy & Astrophysics, 450, 1051–1059 (2006)
Blue Stragglers
New Study Can't Explain Blue Stragglers' Youth | The
Institute for Creation Research
Blue stragglers, according to
NASA, "are older stars that acquire a new lease on life when they collide
and merge with other stars."1 But a new study calls into
question whether stellar collisions can account for these remarkable stars. And
blue stars burn their fuel so quickly that they actually look
young.
Since their discovery,
evolutionary astronomers have sought a way to explain how these stars can even
exist. They burn fuel so fast that they should have burned out billions of
years ago. American astronomers Aaron Geller and Robert Mathieu published in Nature a
description of their model for how older stars could have acquired a "new
lease on life" by siphoning matter from nearby gas giant stars through
"mass transfer."2
They investigated stars within
a cluster called NGC 188, found in the constellation Cepheus. It contains 21
blue stragglers, 16 of which are binary stars that closely interact with nearby
stars. The researchers suspected that the blue stragglers' partners were white
dwarfs, which would be small, leftover remnants of larger red stars that the
blue ones had drained of fuel. Such dwarfs are too faint for direct
observation, but they have sufficient mass to cause their partner stars to
wobble.
Of the 16 binaries, 12 had
rotational periods right at 1,000 days and were thus called
"long-period" blue stragglers. The study authors ran a statistical
analysis that showed "the theoretical and observed [mass] distributions
are indistinguishable."2 In other words, their theory that
other stars "fed" these 12 blue stragglers matched well with what
they observed.
But did this reconcile the
relative youthfulness of these binary blue stars with their assumed billions of
years of history? The answer is no. The authors wrote, "Blue straggler
stars…should already have evolved into giant stars and stellar remnants,"2 and
their new observations do not solve this deep-time problem.
Blue stragglers should burn
through all their fuel in "a few million years at best."3 But
these NGC 188 stars are supposed to be seven billion years old. So, to make
them fit that age, these authors maintain that they were not initially blue stars, but instead burned fuel at a normal rate for billions
of years. Then suddenly, within the last one million years, all 12 of them
began siphoning extra fuel from their binary partners so that they only look young
right now.
However, nothing explains the
many blue stragglers that are not binary stars and yet exist near and far
throughout the universe. Could they have received recent
"youthfulness" through collisions with other stars?
In an article summarizing the
Geller and Mathieu paper, University of Cambridge astronomer Christopher Tout
wrote, "Thus, in this cluster [NGC 188], a collisional origin for blue
stragglers is much rarer than expected, and the authors' study casts doubt on
whether it occurs at all."4 The modelled scenario in which
blue stars form by collision did not match observations.
So, isolated blue stars could
not have received their young looks from a binary system, since by definition they have no binary from which to siphon fuel.
They probably didn't receive their youthful appearance from collisions, either,
according to these results. And though the binary blue stragglers may have
siphoned fuel from nearby partners, the idea that 12 of 16 only did so
recently—after an imagined 7-billion-year wait—defies reasonable odds.
Thus, the best explanation is
still the most straightforward one—blue straggler stars look young because
they are young.
References
|
Cluster |
MYR'S |
BLUE |
YELLOW |
Cluster |
MYR'S |
BLUE |
YELLOW |
|
NGC_2477 |
708 |
5 |
4 |
NGC_5823 |
794 |
|
1 |
|
Berkeley_104 |
776 |
1 |
|
Harvard_8 |
562 |
1 |
|
|
Berkeley_12 |
3,981 |
13 |
|
IC_1311 |
1,585 |
5 |
1 |
|
Berkeley_14 |
1,585 |
9 |
|
IC_166 |
1,000 |
9 |
2 |
|
Berkeley_17 |
10,000 |
20 |
|
IC_361 |
51 |
2 |
|
|
Berkeley_18 |
4,266 |
32 |
|
IC_4651 |
1,122 |
5 |
1 |
|
Berkeley_19 |
2,512 |
13 |
3 |
King_11 |
1,096 |
18 |
|
|
Berkeley_20 |
6,026 |
6 |
3 |
King_19 |
355 |
1 |
|
|
Berkeley_21 |
2,188 |
20 |
|
King_2 |
6,026 |
26 |
2 |
|
Berkeley_22 |
3,311 |
3 |
|
King_5 |
1,259 |
4 |
3 |
|
Berkeley_23 |
794 |
8 |
3 |
King_7 |
661 |
7 |
1 |
|
Berkeley_29 |
1,047 |
1 |
1 |
King_8 |
407 |
3 |
|
|
Berkeley_31 |
2,042 |
6 |
|
Melotte_105 |
355 |
1 |
|
|
Berkeley_32 |
5,012 |
27 |
2 |
Melotte_066 |
3,388 |
14 |
1 |
|
Berkeley_33 |
794 |
1 |
|
Melotte_071 |
234 |
5 |
|
|
Berkeley_39 |
7,943 |
18 |
2 |
NGC_1193 |
5,012 |
12 |
2 |
|
Berkeley_58 |
295 |
1 |
|
NGC_1245 |
1,072 |
5 |
1 |
|
Berkeley_69 |
891 |
1 |
1 |
NGC_1342 |
447 |
1 |
|
|
Berkeley_70 |
4,677 |
12 |
1 |
NGC_1444 |
91 |
2 |
|
|
Berkeley_81 |
1,000 |
1 |
2 |
NGC_1798 |
1,778 |
27 |
2 |
|
Cluster |
MYR'S |
BLUE |
YELLOW |
Cluster |
MYR'S |
BLUE |
YELLOW |
|
Berkeley_99 |
3,162 |
5 |
1 |
NGC_1817 |
407 |
3 |
|
|
Collinder_110 |
1,413 |
8 |
|
NGC_0188 |
7,586 |
22 |
|
|
Collinder_261 |
8,913 |
53 |
3 |
NGC_1907 |
316 |
1 |
|
|
Collinder_74 |
1,288 |
5 |
|
NGC_1912 |
316 |
1 |
|
|
Gulliver_1 |
1,349 |
3 |
|
NGC_2099 |
347 |
1 |
|
|
Gulliver_4 |
1,445 |
4 |
|
NGC_2112 |
1,778 |
4 |
|
|
Gulliver_55 |
1,585 |
3 |
|
NGC_2141 |
1,698 |
18 |
3 |
|
Haffner_6 |
661 |
1 |
|
NGC_2158 |
1,047 |
39 |
3 |
|
NGC_2192 |
1,413 |
1 |
1 |
NGC_2168 |
178 |
1 |
|
|
NGC_2204 |
776 |
7 |
2 |
NGC_6005 |
1,202 |
3 |
|
|
NGC_2243 |
1,072 |
14 |
1 |
NGC_6025 |
76 |
1 |
|
|
NGC_2259 |
316 |
4 |
|
NGC_6067 |
117 |
2 |
1 |
|
NGC_2266 |
631 |
1 |
|
NGC_6124 |
138 |
2 |
|
|
NGC_2324 |
447 |
1 |
|
NGC_6134 |
891 |
4 |
|
|
NGC_2354 |
1,514 |
5 |
1 |
NGC_6253 |
5,012 |
14 |
3 |
|
NGC_2360 |
631 |
1 |
|
NGC_6475 |
295 |
1 |
|
|
NGC_2383 |
282 |
1 |
|
NGC_6583 |
1,000 |
1 |
|
|
NGC_2420 |
1,995 |
3 |
|
NGC_6603 |
562 |
4 |
|
|
NGC_2422 |
72 |
1 |
|
NGC_6633 |
417 |
1 |
|
|
NGC_2437 |
251 |
1 |
3 |
NGC_6705 |
251 |
2 |
1 |
|
NGC_2447 |
380 |
1 |
|
NGC_6791 |
8,318 |
48 |
|
|
NGC_2506 |
1,000 |
14 |
|
NGC_6819 |
2,291 |
15 |
|
|
NGC_2516 |
112 |
1 |
|
NGC_6866 |
813 |
1 |
|
|
NGC_2533 |
692 |
1 |
|
NGC_6939 |
1,585 |
2 |
|
|
NGC_2627 |
1,413 |
3 |
|
NGC_6940 |
708 |
2 |
|
|
NGC_2632 |
741 |
1 |
|
NGC_7044 |
1,259 |
7 |
|
|
NGC_2660 |
1,072 |
2 |
|
NGC_7142 |
3,548 |
10 |
1 |
|
NGC_2682 |
2,818 |
11 |
2 |
NGC_0752 |
1,445 |
|
1 |
|
NGC_2818 |
417 |
5 |
|
NGC_7789 |
3,311 |
16 |
|
|
NGC_2849 |
1,000 |
2 |
|
NGC_7790 |
55 |
1 |
|
|
NGC_3114 |
123 |
|
1 |
Pismis_3 |
1,047 |
4 |
1 |
|
NGC_3680 |
1,175 |
1 |
1 |
Ruprecht_75 |
1,413 |
1 |
3 |
|
NGC_3960 |
1,259 |
2 |
|
Tombaugh_2 |
1,023 |
27 |
2 |
|
NGC_4815 |
229 |
1 |
|
Trumpler_20 |
1,288 |
12 |
1 |
|
NGC_5168 |
100 |
6 |
|
Trumpler_05 |
3,981 |
103 |
2 |
|
NGC_0559 |
224 |
1 |
|
Trumpler_09 |
100 |
1 |
|
|
NGC_5822 |
891 |
1 |
|
Waterloo_7 |
58 |
1 |
|
https://www.aanda.org/articles/aa/pdf/2021/06/aa40072-20.pdf
Astronomy & Astrophysics, 650, A67 (2021)
https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/650/A67
Carbon Stars
The asymptotic giant branch (AGB) is
a region of the Hertzsprung–Russell diagram populated
by evolved cool luminous stars.
This is a period of stellar
evolution undertaken by all low- to
intermediate-mass stars (about 0.5 to 8 solar masses)
late in their lives.
A carbon star (C-type star) is typically an asymptotic giant branch star, a luminous red giant, whose atmosphere contains more carbon than oxygen. The two elements combine in the upper layers of the star, forming carbon monoxide, which consumes most of the oxygen in the atmosphere, leaving carbon atoms free to form other carbon compounds, giving the star a "sooty" atmosphere and a strikingly ruby red appearance. There are also some dwarf and supergiant carbon stars, with the more common giant stars sometimes being called classical carbon stars to distinguish them. [Carbon star - Wikipedia] These stars are ejecting matter at a high rate and thus have a very short life.
|
|
Maximum
Age |
Minimum
Age |
|
|
Years |
Years |
|
Average |
1,522,254 |
45,668 |
|
Maximum |
22,727,273 |
681,818 |
|
Minimum |
74,074 |
2,222 |
|
No. Dates |
307 |
307 |
https://www.aanda.org/articles/aa/pdf/2002/29/aah3520.pdf
Astronomy & Astrophysics, 390, 511–522 (2002)
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/A%2bA/390/511/
|
˙M[M⊙yr] |
Mi/M⊙ |
M∗/M⊙ |
Age/ Years |
Maximum |
Future |
|
Mass/Year |
Original Mass |
Current Mass |
Evolutionary |
Age |
Lifespan |
|
0.0000025 |
1.83 |
1.4 |
1,730,000,000 |
172,000 |
560,000 |
|
0.0000039 |
2.47 |
2 |
824,000,000 |
120,513 |
512,821 |
|
0.0000074 |
1.95 |
1.51 |
1,530,000,000 |
59,459 |
204,054 |
|
0.0000046 |
1.54 |
0.65 |
2,660,000,000 |
193,478 |
141,304 |
|
0.000017 |
2.76 |
2.17 |
598,000,000 |
34,706 |
127,647 |
|
0.0000044 |
1.21 |
0.84 |
6,500,000,000 |
84,091 |
190,909 |
|
0.0000067 |
1.56 |
1.14 |
2,660,000,000 |
62,687 |
170,149 |
|
0.0000081 |
1.74 |
0.66 |
2,010,000,000 |
133,333 |
81,481 |
|
0.0000061 |
1.31 |
0.92 |
4,870,000,000 |
63,934 |
150,820 |
|
0.00001 |
1.67 |
1.21 |
2,350,000,000 |
46,000 |
121,000 |
|
0.000011 |
1.67 |
0.73 |
2,350,000,000 |
85,455 |
66,364 |
|
0.000021 |
2.55 |
1.64 |
825,000,000 |
43,333 |
78,095 |
|
0.000012 |
1.41 |
0.94 |
3,750,000,000 |
39,167 |
78,333 |
|
0.000011 |
1.48 |
0.76 |
2,970,000,000 |
65,455 |
69,091 |
|
0.000011 |
1.48 |
0.75 |
2,970,000,000 |
66,364 |
68,182 |
|
0.000019 |
1.48 |
0.92 |
2,970,000,000 |
29,474 |
48,421 |
|
0.000018 |
1.68 |
0.81 |
2,170,000,000 |
48,333 |
45,000 |
|
0.000039 |
2.46 |
1.38 |
825,000,000 |
27,692 |
35,385 |
|
0.000036 |
2.16 |
1.11 |
1,270,000,000 |
29,167 |
30,833 |
|
0.000083 |
2.66 |
1.31 |
700,000,000 |
16,265 |
15,783 |
https://www.aanda.org/articles/aa/pdf/2003/04/aah3779.pdf
Astronomy & Astrophysics, 398, 229–237 (2003)
.
|
No. |
Mass |
Annual Loss |
Maximum Age |
No. |
Mass |
Annual Loss |
Maximum Age |
|
1 |
0.63 |
0.00003 |
21,000 |
30 |
0.8 |
0.000009 |
88,889 |
|
2 |
0.63 |
0.0000058 |
108,621 |
31 |
0.8 |
0.0000083 |
96,386 |
|
3 |
0.63 |
0.000014 |
45,000 |
32 |
0.8 |
0.00001 |
80,000 |
|
4 |
0.7 |
0.000062 |
11,290 |
33 |
0.8 |
0.000017 |
47,059 |
|
5 |
0.7 |
0.00001 |
70,000 |
34 |
0.8 |
0.00003 |
26,667 |
|
6 |
0.7 |
0.000006 |
116,667 |
35 |
0.8 |
0.000041 |
19,512 |
|
7 |
0.8 |
0.00011 |
7,273 |
36 |
0.84 |
0.000079 |
10,633 |
|
8 |
0.8 |
0.000014 |
57,143 |
37 |
0.84 |
0.00002 |
42,000 |
|
9 |
0.8 |
0.000006 |
133,333 |
38 |
0.84 |
0.000011 |
76,364 |
|
10 |
0.8 |
0.0000049 |
163,265 |
39 |
0.94 |
0.000088 |
10,682 |
|
11 |
0.8 |
0.0000065 |
123,077 |
40 |
0.94 |
0.000023 |
40,870 |
|
12 |
0.8 |
0.0000074 |
108,108 |
41 |
0.94 |
0.000012 |
78,333 |
|
13 |
0.8 |
0.0000064 |
125,000 |
42 |
0.94 |
0.000025 |
37,600 |
|
14 |
0.8 |
0.000013 |
61,538 |
43 |
1 |
0.000026 |
38,462 |
|
15 |
0.8 |
0.000013 |
61,538 |
44 |
1 |
0.000059 |
16,949 |
|
16 |
0.8 |
0.000016 |
50,000 |
45 |
1 |
0.000077 |
12,987 |
|
17 |
0.8 |
0.000016 |
50,000 |
46 |
1 |
0.000079 |
12,658 |
|
18 |
0.8 |
0.000019 |
42,105 |
47 |
1 |
0.000043 |
23,256 |
|
19 |
0.8 |
0.00001 |
80,000 |
48 |
1 |
0.000026 |
38,462 |
|
20 |
0.8 |
0.000025 |
32,000 |
49 |
1 |
0.0000046 |
217,391 |
|
21 |
0.8 |
0.000051 |
15,686 |
50 |
1 |
0.0000054 |
185,185 |
|
22 |
0.8 |
0.000036 |
22,222 |
51 |
1 |
0.0000051 |
196,078 |
|
23 |
0.8 |
0.00005 |
16,000 |
52 |
1 |
0.000018 |
55,556 |
|
24 |
0.8 |
0.00007 |
11,429 |
53 |
1 |
0.000013 |
76,923 |
|
25 |
0.8 |
0.000099 |
8,081 |
54 |
1 |
0.0000096 |
104,167 |
|
26 |
0.8 |
0.0000039 |
205,128 |
55 |
1.2 |
0.0000061 |
196,721 |
|
27 |
0.8 |
0.0000056 |
142,857 |
56 |
1.2 |
0.000013 |
92,308 |
|
28 |
0.8 |
0.0000061 |
131,148 |
57 |
1.2 |
0.000016 |
75,000 |
|
29 |
0.8 |
0.0000038 |
210,526 |
58 |
1.2 |
0.0000098 |
122,449 |
https://www.aanda.org/articles/aa/pdf/2002/11/aah3281.pdf
Astronomy & Astrophysics, 384, 452–459 (2002)
.
Investigation of the mass loss mechanism
https://ui.adsabs.harvard.edu/abs/2000A%26A...361..641W/abstract
|
|
Maximum
Age |
Minimum
Age |
Remaining
Life |
|
|
Years |
Years |
Years |
|
Average |
5,979,950 |
516,624 |
717,549 |
|
Maximum |
370,000,000 |
26,666,667 |
33,333,333 |
|
Minimum |
257,576 |
33,333 |
45,455 |
|
No. Dates |
325 |
325 |
325 |
https://www.aanda.org/articles/aa/pdf/2010/01/aa12084-09.pdf
Astronomy & Astrophysics, 509, A14 (2010)
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/A%2bA/509/A14
Mass loss is a crucial process that affects the observational properties, evolution path, and fate of highly evolved
stars. However, the mechanism of mass loss is still unclear, and the mass-loss rate (MLR) of red supergiant stars
(RSGs) requires further research and precise evaluation. To address this, we utilized an updated and complete
sample of RSGs in the Large Magellanic Cloud (LMC) and employed the 2-DUST radiation transfer model and
spectral energy distribution fitting approach to determine the dust-production rates (DPRs) and dust properties of
the RSGs. We have fitted 4714 selected RSGs with over 100,000 theoretical templates of evolved stars. Our results
show that the DPR range of RSGs in the LMC is 10−11Me yr−1–10−7Me yr−1, and the total DPR of all RSGs is
1.14 ×10−6Me yr−1. [The Astronomical Journal, Volume 167, Issue 2, id.51]
|
|
Age |
|
|
Years |
|
Average |
4,384 |
|
Maximum |
63,000 |
|
Minimum |
776 |
|
No. Dates |
4,717 |
https://iopscience.iop.org/article/10.3847/1538-3881/ad12bf/pdf
The Astronomical Journal, Volume 167, Issue 2, id.51
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/167/51
The PACS observations show extended emission at both wavelengths: at 70 μm, we observe extended emission at 3σ brightness
levels from 0.04 to 0.74 pc averaging at 0.16±0.04 pc. The observations allowed us to observe the mass-loss histories up to an average
of 9000 ± 1100 yr, ranging from 4500–21800 yr. At 160 μm, R3σ and lookback time-averaged 0.011 ± 0.02 pc and 6500 ± 1000 yr,
respectively. At both PACS wavelengths, the circumstellar shell structure and extended emission we measured are consistent with
the results from Cox et al.
|
Source |
Age, Years |
Age, Years |
|
Star |
Dust |
Gas |
|
CIT6 |
7,066 |
7,057 |
|
EPAqr |
1,199 |
963 |
|
IKTau |
6,558 |
6,821 |
|
IRC+10011 |
11,783 |
12,073 |
|
IRC+10216 |
11,373 |
11,123 |
|
LPAnd |
9,489 |
9,323 |
|
NMLCyg |
8,922 |
8,877 |
|
oCeti |
5,036 |
4,967 |
|
RCas |
5,345 |
5,341 |
|
RLeo |
1,337 |
1,313 |
|
RXBoo |
3,189 |
3,177 |
|
TXCam |
2,438 |
2,337 |
|
UHya |
14,448 |
14,639 |
|
WAql |
4,426 |
4,383 |
|
WHya |
4,988 |
5,246 |
|
IRC+10216 |
11,295 |
11,123 |
https://doi.org/10.1093/mnras/sty1422
MNRAS, 479, 536–552 (2018)
Magnetar Spin
A magnetar is a type of neutron
star with an extremely powerful magnetic
field (~109 to 1011 T,
~1013 to 1015 G). The
magnetic-field decay (or dissipation) powers the emission of high-energy electromagnetic radiation,
particularly X-rays and gamma rays.
The existence of magnetars was proposed in 1992 by Robert Duncan and Christopher Thompson, who sought to explain the properties of transient sources of gamma rays, now known as soft gamma repeaters (SGRs). Over the following decade, the magnetar hypothesis became widely accepted, and was extended to explain anomalous X-ray pulsars (AXPs). Out of approximately 3,000 neutron stars, there are 31 confirmed magnetars of which five are both magnetars and pulsars, as of January 2021. They have very short lives.
|
Magnetar |
|||
|
|
Name |
Magnetar |
1,000
Years |
|
CXOU
J010043.1-721134 |
YES |
6.8 |
|
|
4U
0142+61 |
YES |
68 |
|
|
SGR
0418+5729 |
YES |
36,000 |
|
|
SGR
0501+4516 |
YES |
16 |
|
|
SGR
0526-66 |
YES |
3.4 |
|
|
1E
1048.1-5937 |
YES |
4.5 |
|
|
1E
1547.0-5408 |
YES |
0.69 |
|
|
PSR
J1622-4950 |
YES |
4 |
|
|
SGR
1627-41 |
YES |
2.2 |
|
|
CXOU
J164710.2-455216 |
YES |
420 |
|
|
1RXS
J170849.0-400910 |
YES |
9.1 |
|
|
CXOU
J171405.7-381031 |
YES |
0.95 |
|
|
SGR
J1745-2900 |
YES |
9 |
|
|
SGR
1806-20 |
YES |
0.24 |
|
|
XTE
J1810-197 |
YES |
11 |
|
|
Swift
J1822.3-1606 |
YES |
440 |
|
|
SGR
1833-0832 |
YES |
34 |
|
|
Swift
J1834.9-0846 |
YES |
4.9 |
|
|
1E
1841-045 |
YES |
4.7 |
|
|
SGR
1900+14 |
YES |
0.9 |
|
|
1E
2259+586 |
YES |
230 |
|
|
SGR
1801-23 |
NO |
|
|
|
SGR
1808-20 |
NO |
|
|
|
AX
J1818.8-1559 |
NO |
|
|
|
AX
J1845.0-0258 |
NO |
|
|
|
SGR
2013+34 |
NO |
|
https://iopscience.iop.org/article/10.1088/0067-0049/212/1/6
The Astrophysical Journal Supplement, 212:6, 2014
.
|
Name |
A |
A |
B |
B |
C |
C |
D |
D |
Notes |
|
CXOU J010043.1−721134 |
6.8 |
|
14 |
|
|
|
|
|
SMC |
|
4U 0142+61 |
68 |
|
0.3 |
|
|
|
|
|
|
|
SGR 0418+5729 |
3,600 |
|
220 |
|
|
|
|
|
|
|
SGR 0501+4516 |
15 |
|
99 |
|
|
|
4 |
7 |
SNR (G160.9+02.6) |
|
SGR 0526−66 |
1.9 |
3.4 |
10 |
17 |
26 |
44 |
4.8 |
|
LMC |
|
1E 1048.1−5937 |
2 |
8 |
10 |
40 |
|
|
|
|
|
|
(PSR J1119−6127) |
1.6 |
|
0.02 |
|
|
|
4.2 |
7.1 |
SNR (G292.2−0.5) |
|
1E 1547.0−5408 |
0.7 |
1.4 |
220 |
460 |
|
|
|
|
SNR (G327.24−0.13) |
|
PSR J1622−4950 |
3.5 |
7.3 |
550 |
1,100 |
|
|
6 |
|
SNR (G333.9+00.0) |
|
SGR 1627−41 |
2.2 |
|
83 |
|
|
|
5 |
|
SNR (G337.0−00.1) |
|
CXOU J164710.2−455216 |
173 |
|
138 |
|
|
|
|
|
Westerlund |
|
1RXS J170849.0−400910 |
9 |
|
9.3 |
|
|
|
|
|
2,42,43 |
|
CXOU J171405.7−381031 |
0.58 |
1 |
24 |
43 |
|
|
0.35 |
3.15 |
SNR (CTB 37B) |
|
SGR J1745−2900 |
4.3 |
9.7 |
2,800 |
|
|
|
|
|
Galactic centre |
|
SGR 1806−20 |
0.16 |
1.45 |
6.1 |
55 |
0.6 |
5.3 |
|
|
W31 |
|
XTE J1810−197 |
8.4 |
20 |
3,000 |
8,000 |
|
|
|
|
|
|
Swift J1822.3−1606 |
1,600 |
6,400 |
2,600 |
|
|
|
|
|
|
|
SGR 1833−0832 |
34 |
|
|
|
|
|
|
|
|
|
Swift J1834.9−0846 |
4.9 |
|
1,400 |
|
|
|
|
|
|
|
1E 1841−045 |
4.5 |
|
5.9 |
|
|
|
0.75 |
2.1 |
SNR (Kes 73) |
|
(PSR J1846−0258) |
0.73 |
|
0.05 |
|
|
|
0.35 |
0.56 |
SNR (Kes 75) |
|
3XMM J185246.6+003317 |
1,300 |
|
|
|
|
|
4.4 |
6.7 |
SNR (G033.6+00.1) |
|
SGR 1900+14 |
0.46 |
1.3 |
8.8 |
25 |
30 |
83 |
|
|
26,37,38,39 |
|
SGR 1935+2154 |
3.6 |
|
|
|
|
|
41 |
|
SNR (G57.2+0.8) |
|
1E 2259+586 |
230 |
|
1.2 |
|
|
|
9 |
|
SNR (CTB 109) |
|
A |
Dipole spin-down age |
1,000 Years |
|
B |
Magnetic field decay age from
persistent emission |
1,000 Years |
|
C |
Magnetic field decay age from GF
emission, assuming one GF every 50 yr |
1,000 Years |
|
D |
SNR age estimate |
1,000 Years |
https://doi.org/10.1093/mnras/stz1391
MNRAS 487, 1426–1438 (2019)
.
Nucleosynthesis
Impossible dates. Older
than Big Bang/Negative ages.
|
Galaxy |
Age |
Galaxy |
Age |
|
Name |
Gyr |
Name |
Gyr |
|
NGC
3078 |
14 |
NGC
4105 |
>17 |
|
NGC
4106 |
14 |
NGC
4464 |
>17 |
|
IC
4045 |
14 |
NGC
5582 |
>17 |
|
ESO
539-G11 |
14 |
NGC
5813 |
>17 |
|
NGC
4261 |
14.4 |
NGC
6736 |
>17 |
|
NGC
1419 |
14.5 |
NGC
6849 |
>17 |
|
NGC
1209 |
15 |
NGC
7768 |
>17 |
|
NGC
4839 |
15 |
IC
0843 |
>17 |
|
NGC
4869 |
15 |
IC
3947 |
>17 |
|
NGC
0936 |
16 |
IC
5105 |
>17 |
|
NGC
4458 |
16 |
IC
5328 |
>17 |
|
IC
5358 |
16 |
IC
5364N2 |
>17 |
|
NGC
1210 |
>17 |
ESO
283-G19 |
>17 |
|
NGC
1553 |
>17 |
ESO
297-G34 |
>17 |
|
NGC
2329 |
>17 |
ESO
486-G29 |
>17 |
|
NGC
2945 |
>17 |
ESO
507-G46 |
>17 |
|
NGC
3051 |
>17 |
ESO
545-G40 |
>17 |
https://doi.org/10.1046/j.1365-8711.2002.05073.x
MNRAS, 330, 547–562 (2002)
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/MNRAS/330/547
Impossible dates. Older
than Big Bang/Negative ages.
|
Star Cluster |
Age, Years |
Age, Years |
|
B001-G039 |
6,309,573,445 |
17,782,794,100 |
|
B002-G043 |
7,244,359,601 |
11,220,184,543 |
|
B003-G045 |
17,378,008,287 |
4,168,693,835 |
|
B004-G050 |
18,620,871,367 |
15,488,166,189 |
|
B005-G052 |
8,317,637,711 |
17,782,794,100 |
|
B006-G058 |
8,317,637,711 |
10,000,000,000 |
|
B008-G060 |
8,317,637,711 |
17,782,794,100 |
|
B010-G062 |
4,897,788,194 |
4,897,788,194 |
|
B011-G063 |
15,488,166,189 |
8,511,380,382 |
|
B011D___ |
4,168,693,835 |
5,370,317,964 |
|
B012-G064 |
12,022,644,346 |
11,748,975,549 |
|
LAMOST-1 |
9,332,543,008 |
14,454,397,707 |
|
LAMOST-2 |
14,454,397,707 |
17,782,794,100 |
|
LAMOST-3 |
6,025,595,861 |
11,748,975,549 |
|
LAMOST-4 |
19,952,623,150 |
12,302,687,708 |
|
LAMOST-5 |
14,791,083,882 |
8,912,509,381 |
https://doi.org/10.3847/0004-6256/152/2/45
The Astronomical Journal, 152:45, 2016
.
Impossible dates. Older
than Big Bang/Negative ages.
|
RGB-Age |
RC-Age |
RGB-Age, Nom |
RC-Age, Nom |
YREC-Age |
|
|
|
Gyr |
Gyr |
Gyr |
Gyr |
Gyr |
|
Max Age |
67 |
61 |
68 |
67 |
86 |
|
Min Age |
15 |
15 |
15 |
15 |
15 |
|
No. Dates |
336 |
240 |
352 |
842 |
494 |
https://iopscience.iop.org/article/10.3847/1538-4365/ad9fef/pdf
The Astrophysical Journal Supplement Series, 276:69, 2025
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/ApJS/276/69
|
|
Billion Years |
Billion Years |
Billion Years |
|
Average |
32.84 |
27.55 |
13.46 |
|
Maximum |
651.13 |
149.03 |
17.66 |
|
Minimum |
13.07 |
13.09 |
4.46 |
|
No. Dates |
139 |
129 |
129 |
https://iopscience.iop.org/article/10.3847/1538-3881/abd39d/pdf
The Astronomical Journal, 161:100, 2021
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AJ/161/100
Impossible dates. Older
than Big Bang/Negative ages.
|
|
Billion Years |
|
|
|
|
Average |
25.93 |
|
Maximum |
602.55 |
|
Minimum |
15.13 |
|
No. Dates |
5793 |
https://iopscience.iop.org/article/10.3847/1538-4357/abaeee/pdf
The Astrophysical Journal, 901:109, 2020
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/901/109
Impossible dates. Older
than Big Bang/Negative ages.
|
Star |
Billion Years |
Star |
Billion Years |
|
BD+08_2856 |
13.5 |
HD108577 |
14 |
|
BD+17_3248 |
8.4 |
HD204543 |
14 |
|
HD122563 |
-30.3 |
M15-K341 |
14 |
|
HD88609 |
-27 |
M15-K462 |
16.8 |
|
HE0338-3945 |
-25 |
HE2148-1247 |
>15.9 |
|
CS30306-132 |
-16.3 |
HD126587 |
>4.2 |
|
CS31078-018 |
-7 |
HD128279 |
>4.7 |
|
CS31082-001 |
-5.1 |
BD+04_2621 |
>8.4 |
|
HE1219-0312 |
-4.7 |
|
|
|
M5-IV-81 |
-2.8 |
|
|
|
CS29497-004 |
-2.3 |
|
|
|
BD-18_5550 |
-0.9 |
|
|
https://arxiv.org/pdf/1112.4870
Astronomy & Astrophysics, 537, A118 (2012)
Metallicity
estimates for old star clusters in M 33
Impossible dates. Older
than Big Bang/Negative ages.
|
Cluster |
Age, Years |
|
CBF11 |
19,952,623,150 |
|
CBF97 |
19,054,607,180 |
|
CBF161 |
19,054,607,180 |
|
U137 |
18,620,871,367 |
|
M5 |
17,378,008,287 |
https://www.aanda.org/articles/aa/pdf/2004/02/aa3620.pdf Astronomy & Astrophysics,
413,563–570(2004)
.
Impossible dates. Older
than Big Bang/Negative ages.
|
|
Billion Years |
|
Average |
48.56 |
|
Maximum |
302,141 |
|
Minimum |
15.01 |
|
No. Dates |
17,004 |
https://www.aanda.org/articles/aa/pdf/2023/07/aa45809-22.pdf
Astronomy & Astrophysics, A675, A26 (2023)
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/675/A26
Impossible dates. Older
than Big Bang/Negative ages.
|
|
Billion Years |
Billion Years |
Billion Years |
Billion Years |
|
Max Age |
38 |
37 |
41 |
38 |
|
Min Age |
20 |
20 |
20 |
20 |
|
No. Dates |
6,069 |
229 |
104 |
8,782 |
|
Max Age |
38 |
104 |
98 |
93 |
|
Min Age |
20 |
20 |
20 |
20 |
|
No. Dates |
8,724 |
8,590 |
5,169 |
360 |
|
Max Age |
-0.001 |
-0.001 |
-0.001 |
|
|
Min Age |
-24.717 |
-24.688 |
-7.913 |
|
|
No. Dates |
221,667 |
11,149 |
14,996 |
|
|
Max Age |
80 |
96 |
40 |
40 |
|
Min Age |
20 |
20 |
20 |
20 |
|
No. Dates |
1,044 |
20,425 |
12,321 |
13,353 |
|
Max Age |
66 |
66 |
69 |
|
|
Min Age |
20 |
20 |
20 |
|
|
No. Dates |
60,063 |
60,511 |
48,291 |
|
https://www.aanda.org/articles/aa/pdf/2026/04/aa58436-25.pdf
Astronomy & Astrophysics, 708, A215 (2026)
https://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/A%2bA/708/A215/
Impossible dates. Older
than Big Bang/Negative ages.
|
Gyr's |
Gyr's |
Gyr's |
Gyr's |
|
3.1 |
5.3 |
0 |
-5 |
|
7.8 |
14.8 |
18.1 |
18.3 |
|
10.5 |
18.8 |
23.8 |
27.5 |
|
|
21.1 |
27.9 |
32.5 |
|
11 |
22.8 |
30.1 |
38.5 |
|
|
24 |
31 |
43.5 |
|
|
24.5 |
|
42.5 |
|
|
12 |
23.8 |
29.8 |
|
|
22.1 |
|
|
|
13.2 |
20.8 |
27 |
34.8 |
|
|
|
25.5 |
|
|
|
19.1 |
25.3 |
37.5 |
|
15.1 |
|
26 |
|
|
|
19.2 |
|
|
|
16.9 |
20.3 |
29.5 |
45 |
|
|
|
|
|
|
19.3 |
24 |
35 |
|
|
|
|
40 |
|
https://onlinelibrary.wiley.com/doi/epdf/10.1002/asna.70056
Astronomische Nachrichten, 2026; 347:e70056
Red Super Giants
These stars are ejecting matter at a high rate and thus have a
very short life.
|
Initial Mass |
Final Mass |
Mass Lost |
Annual Loss |
Age |
Years Left |
|
25 |
9.6199 |
15.3801 |
4.450E-04 |
34,562 |
21,618 |
|
20 |
7.1887 |
12.8113 |
2.370E-04 |
54,056 |
30,332 |
|
25 |
8.2843 |
16.7157 |
2.560E-04 |
65,296 |
32,361 |
|
25 |
9.7153 |
15.2847 |
1.950E-04 |
78,383 |
49,822 |
|
20 |
6.5014 |
13.4986 |
1.270E-04 |
106,288 |
51,192 |
|
25 |
8.2648 |
16.7352 |
1.300E-04 |
128,732 |
63,575 |
|
20 |
7.2971 |
12.7029 |
8.700E-05 |
146,010 |
83,875 |
|
15 |
5.3091 |
9.6909 |
4.570E-05 |
212,055 |
116,173 |
|
25 |
9.6896 |
15.3104 |
7.170E-05 |
213,534 |
135,141 |
|
20 |
6.6413 |
13.3587 |
5.000E-05 |
267,174 |
132,826 |
|
15 |
4.6011 |
10.3989 |
3.040E-05 |
342,069 |
151,352 |
|
15 |
5.3064 |
9.6936 |
1.960E-05 |
494,571 |
270,735 |
|
20 |
7.1785 |
12.8215 |
2.540E-05 |
504,783 |
282,618 |
|
20 |
8.6347 |
11.3653 |
1.620E-05 |
701,562 |
533,006 |
|
15 |
4.8563 |
10.1437 |
1.320E-05 |
768,462 |
367,902 |
|
15 |
13.1739 |
1.8261 |
1.500E-06 |
1,217,400 |
8,782,600 |
|
25 |
8.2893 |
16.7107 |
1.340E-05 |
1,247,067 |
618,604 |
|
15 |
11.5156 |
3.4844 |
2.560E-06 |
1,361,094 |
4,498,281 |
|
9 |
8.5175 |
0.4825 |
1.780E-07 |
2,710,674 |
47,851,124 |
|
9 |
8.7651 |
0.2349 |
8.660E-08 |
2,712,471 |
101,213,626 |
|
9 |
2.5951 |
6.4049 |
1.930E-06 |
3,318,601 |
1,344,611 |
|
9 |
3.4715 |
5.5285 |
1.580E-06 |
3,499,051 |
2,197,152 |
|
9 |
6.1108 |
2.8892 |
8.250E-07 |
3,502,061 |
7,407,030 |
|
9 |
6.6876 |
2.3124 |
6.490E-07 |
3,563,020 |
10,304,468 |
https://doi.org/10.1051/0004-6361/201424671
Astronomy & Astrophysics, 575, A60 (2015)
.
These stars are ejecting matter at a high rate and thus have a very short life.
|
Number |
Min Age |
|
Dates |
Years |
|
1184 |
<1,000,000 |
|
Number |
Max Age |
|
Dates |
Years |
|
465 |
<1,000,000 |
https://iopscience.iop.org/article/10.3847/1538-4357/abed4b/pdf
The Astrophysical Journal, 912:112, 2021
http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/912/112
|
STAR'S |
Annual Loss |
Model One |
Model One |
|
NAME |
Log10[x] |
Min Ages |
Max Ages |
|
HV12501 |
-4.79 |
30,830 |
493,276 |
|
HV2360 |
-4.51 |
16,180 |
258,875 |
|
HV2446 |
-5.14 |
69,019 |
1,104,307 |
|
HV2561 |
-4.47 |
14,756 |
236,097 |
|
HV5870 |
-4.68 |
23,932 |
382,904 |
|
HV888 |
-4.43 |
13,458 |
215,323 |
|
HV916 |
-4.5 |
15,811 |
252,982 |
|
HV986 |
-4.89 |
38,812 |
620,998 |
|
HV996 |
-4.28 |
9,527 |
152,437 |
|
IRAS-3008 |
-4.15 |
7,063 |
113,003 |
|
IRAS-2500 |
-4.3 |
9,976 |
159,621 |
|
IRAS-2500 |
-4.45 |
14,092 |
225,471 |
|
IRAS-2667 |
-4.23 |
8,491 |
135,859 |
|
IRAS-2667 |
-4.34 |
10,939 |
175,021 |
|
IRAS-2667 |
-4.36 |
11,454 |
183,269 |
|
IRAS-2890 |
-4.14 |
6,902 |
110,431 |
|
SHV0522023 |
-6.8 |
3,154,787 |
50,476,588 |
|
SHV0530323 |
-5.67 |
233,868 |
3,741,881 |
|
SP77 |
-4.76 |
28,772 |
460,352 |
|
SP77 |
-4.56 |
18,154 |
290,462 |
|
WOHG64 |
-3.12 |
659 |
10,546 |
|
WOHSG374 |
-4.43 |
13,458 |
215,323 |
|
GRV0519-6700 |
-6.2 |
792,447 |
12,679,146 |
|
HV12070 |
-5.2 |
79,245 |
1,267,915 |
|
SHV0524565 |
-6.53 |
1,694,221 |
27,107,532 |
|
J050024.95 |
-5.05 |
56,101 |
897,615 |
|
J050615.14 |
-4.96 |
45,601 |
729,609 |
|
J050659.94 |
-5.64 |
218,258 |
3,492,127 |
|
J050738.74 |
-5.07 |
58,745 |
939,918 |
|
GRV0507 |
-5.59 |
194,523 |
3,112,361 |
|
IRAS-05289 |
-4.35 |
11,194 |
179,098 |
|
SHV0500533 |
-5.39 |
122,735 |
1,963,767 |
|
SHV0504018 |
-5.3 |
99,763 |
1,596,210 |
|
SHV0504266 |
-5.48 |
150,998 |
2,415,961 |
|
SHV0504353 |
-5.62 |
208,435 |
3,334,955 |
|
SP77 |
-5.51 |
161,797 |
2,588,749 |
|
STAR'S |
Loss/Year |
Model One |
Model One |
Loss/Year |
Model Two |
Model Two |
|
NAME |
Log10[x] |
Min Ages |
Max Ages |
Log10[x] |
Min Ages |
Max Ages |
|
S-CrB |
-6.96 |
4,560,054 |
72,960,867 |
-5.66 |
228,544 |
3,656,706 |
|
RLeo |
-7.07 |
5,874,488 |
93,991,804 |
-5.44 |
137,711 |
2,203,383 |
|
RLMi |
-6.82 |
3,303,467 |
52,855,476 |
-5.66 |
228,544 |
3,656,706 |
|
RXBoo |
-6.8 |
3,154,787 |
50,476,588 |
-5.55 |
177,407 |
2,838,507 |
|
WHya |
-7 |
5,000,000 |
80,000,000 |
-5.66 |
228,544 |
3,656,706 |
|
KUAnd |
-4.72 |
26,240 |
419,846 |
-4.91 |
40,642 |
650,264 |
|
WXPsc |
-4.64 |
21,826 |
349,213 |
-4.91 |
40,642 |
650,264 |
|
02316+6455 |
-5.07 |
58,745 |
939,918 |
-4.91 |
40,642 |
650,264 |
|
02351-2711 |
-5.44 |
137,711 |
2,203,383 |
-4.91 |
40,642 |
650,264 |
|
NML |
-5.22 |
82,979 |
1,327,670 |
-5.5 |
158,114 |
2,529,822 |
|
04307+6210 |
-5.44 |
137,711 |
2,203,383 |
-5.5 |
158,114 |
2,529,822 |
|
TXCam |
-5.6 |
199,054 |
3,184,857 |
-5.02 |
52,356 |
837,703 |
|
05411+6957 |
-5.23 |
84,912 |
1,358,595 |
-4.91 |
40,642 |
650,264 |
|
VCam |
-5.66 |
228,544 |
3,656,706 |
-5.34 |
109,388 |
1,750,209 |
|
06300+6058 |
-5.28 |
95,273 |
1,524,369 |
-4.91 |
40,642 |
650,264 |
|
GXMon |
-5.03 |
53,576 |
857,215 |
-4.91 |
40,642 |
650,264 |
|
IWHya |
-5.02 |
52,356 |
837,703 |
-4.91 |
40,642 |
650,264 |
|
V2108 |
-5.42 |
131,513 |
2,104,214 |
-4.91 |
40,642 |
650,264 |
|
V774 |
-5.55 |
177,407 |
2,838,507 |
-5.6 |
199,054 |
3,184,857 |
|
18009-2019 |
-5.37 |
117,211 |
1,875,383 |
-5.12 |
65,913 |
1,054,605 |
|
18135-1641 |
-5.3 |
99,763 |
1,596,210 |
-5.6 |
199,054 |
3,184,857 |
|
18204-1344 |
-5.38 |
119,942 |
1,919,066 |
-5.12 |
65,913 |
1,054,605 |
|
V1111 |
-5.28 |
95,273 |
1,524,369 |
-4.91 |
40,642 |
650,264 |
|
18413+1354 |
-5.26 |
90,985 |
1,455,761 |
-5.34 |
109,388 |
1,750,209 |
|
V3953 |
-5.17 |
73,955 |
1,183,287 |
-4.91 |
40,642 |
650,264 |
|
V3880 |
-5 |
50,000 |
800,000 |
-5.12 |
65,913 |
1,054,605 |
|
V342 |
-5.36 |
114,543 |
1,832,694 |
-4.91 |
40,642 |
650,264 |
|
20440-0105 |
-5.57 |
185,768 |
2,972,282 |
-4.91 |
40,642 |
650,264 |
|
UUPeg |
-5.8 |
315,479 |
5,047,659 |
-5.34 |
109,388 |
1,750,209 |
|
RTCep |
-5.6 |
199,054 |
3,184,857 |
-5.5 |
158,114 |
2,529,822 |
|
23496+6131 |
-5.27 |
93,104 |
1,489,670 |
-4.91 |
40,642 |
650,264 |
|
STAR'S |
Loss/Year |
Model One |
Model One |
Loss/Year |
Model Two |
Model Two |
|
NAME |
Log10[x] |
Min Ages |
Max Ages |
Log10[x] |
Min Ages |
Max Ages |
|
KWSgr |
-5.4 |
125,594 |
2,009,509 |
-4.89 |
38,812 |
620,998 |
|
VXSgr |
-4.4 |
12,559 |
200,951 |
-4.47 |
14,756 |
236,097 |
|
UYSct |
-5.15 |
70,627 |
1,130,030 |
-4.66 |
22,854 |
365,671 |
|
BD+24◦3902 |
-6 |
500,000 |
8,000,000 |
-4.83 |
33,804 |
540,866 |
|
BICyg |
-5.22 |
82,979 |
1,327,670 |
-4.34 |
10,939 |
175,021 |
|
KYCyg |
-5.4 |
125,594 |
2,009,509 |
-4.06 |
5,741 |
91,852 |
|
NML-Cyg |
-4 |
5,000 |
80,000 |
-3.71 |
2,564 |
41,029 |
|
μ-Cep |
-6.05 |
561,009 |
8,976,148 |
-4.15 |
7,063 |
113,003 |
|
PZCas |
-5 |
50,000 |
800,000 |
-4.46 |
14,420 |
230,723 |
|
TZCas |
-5.52 |
165,566 |
2,649,049 |
-4.78 |
30,128 |
482,048 |
|
S-Per |
-5.15 |
70,627 |
1,130,030 |
-4.41 |
12,852 |
205,632 |
|
SUPer |
-5.22 |
82,979 |
1,327,670 |
-4.73 |
26,852 |
429,625 |
|
αOri |
-6.7 |
2,505,936 |
40,094,979 |
-4.83 |
33,804 |
540,866 |
|
VYCMa |
-4 |
5,000 |
80,000 |
-3.92 |
4,159 |
66,541 |
|
EVCar |
-5.22 |
82,979 |
1,327,670 |
-4.34 |
10,939 |
175,021 |
|
CKCar |
-5.7 |
250,594 |
4,009,498 |
-4.69 |
24,489 |
391,823 |
|
IXCar |
-5.05 |
56,101 |
897,615 |
-4.78 |
30,128 |
482,048 |
|
V396-Cen |
-6 |
500,000 |
8,000,000 |
-4.34 |
10,939 |
175,021 |
|
AHSco |
-5.1 |
62,946 |
1,007,140 |
-4.16 |
7,227 |
115,635 |
https://www.aanda.org/articles/aa/pdf/2005/28/aa2555-04.pdf
Astronomy & Astrophysics, 438,273–289(2005)
Wolf-Rayet Stars
Wolf-Rayet stars
These stars are ejecting matter at a high rate and thus have a very short life.
https://www.aanda.org/articles/aa/pdf/2017/12/aa31590-17.pdf
Astronomy & Astrophysics, 608, A34 (2017)
|
Mass |
Annual Loss |
Annual Loss |
Lifespan |
Mass |
Annual Loss |
Annual Loss |
Lifespan |
|
Log[x] |
Sun=1 |
Years |
Log[x] |
Sun=1 |
Years |
||
|
14.57 |
-5.47 |
3.38844E-06 |
4,299,912 |
18.83 |
-4.72 |
1.90546E-05 |
988,212 |
|
23.08 |
-5.25 |
5.62341E-06 |
4,104,269 |
23.08 |
-4.63 |
2.34423E-05 |
984,546 |
|
16.53 |
-5.2 |
6.30957E-06 |
2,619,828 |
13.7 |
-4.84 |
1.44544E-05 |
947,808 |
|
15.51 |
-5.21 |
6.16595E-06 |
2,515,427 |
15.51 |
-4.75 |
1.77828E-05 |
872,191 |
|
12.14 |
-5.27 |
5.37032E-06 |
2,260,574 |
13.7 |
-4.75 |
1.77828E-05 |
770,408 |
|
17.64 |
-4.99 |
1.02329E-05 |
1,723,846 |
17.64 |
-4.63 |
2.34423E-05 |
752,486 |
|
17.64 |
-4.96 |
1.09648E-05 |
1,608,787 |
17.64 |
-4.62 |
2.39883E-05 |
735,358 |
|
15.51 |
-4.94 |
1.14815E-05 |
1,350,865 |
17.64 |
-4.48 |
3.31131E-05 |
532,719 |
|
14.57 |
-4.92 |
1.20226E-05 |
1,211,880 |
12.89 |
-4.54 |
2.88403E-05 |
446,944 |
|
18.83 |
-4.78 |
1.65959E-05 |
1,134,620 |
33.24 |
-4.09 |
8.12831E-05 |
408,941 |
|
12.89 |
-4.94 |
1.14815E-05 |
1,122,672 |
12.14 |
-4.51 |
3.0903E-05 |
392,843 |
|
18.83 |
-4.75 |
1.77828E-05 |
1,058,889 |
20.13 |
-4.28 |
5.24807E-05 |
383,569 |
|
15.51 |
-4.83 |
1.47911E-05 |
1,048,605 |
14.57 |
-4.42 |
3.80189E-05 |
383,230 |
|
13.7 |
-4.88 |
1.31826E-05 |
1,039,251 |
21.54 |
-4.25 |
5.62341E-05 |
383,041 |
|
13.7 |
-4.87 |
1.34896E-05 |
1,015,595 |
21.54 |
-4.22 |
6.0256E-05 |
357,475 |
The Mass-Loss Rates Of Wc And Wo Stars
https://iopscience.iop.org/article/10.3847/1538-4357/833/2/133/pdf
The Astrophysical Journal, 833:133 (6pp), 2016
|
log M |
Years/Solar Mass |
Years/100 Solar Mass |
|
-5.14 |
138,038 |
13,803,843 |
|
-5.10 |
125,893 |
12,589,254 |
|
-5.05 |
112,202 |
11,220,185 |
|
-5.00 |
100,000 |
10,000,000 |
|
-5.00 |
100,000 |
10,000,000 |
|
-4.94 |
87,096 |
8,709,636 |
|
-4.92 |
83,176 |
8,317,638 |
|
-4.90 |
79,433 |
7,943,282 |
|
-4.90 |
79,433 |
7,943,282 |
|
-4.80 |
63,096 |
6,309,573 |
|
-4.80 |
63,096 |
6,309,573 |
|
-4.80 |
63,096 |
6,309,573 |
|
-4.80 |
63,096 |
6,309,573 |
|
-4.76 |
57,544 |
5,754,399 |
|
-4.60 |
39,811 |
3,981,072 |
|
-4.50 |
31,623 |
3,162,278 |
|
-4.50 |
31,623 |
3,162,278 |
|
-4.50 |
31,623 |
3,162,278 |
|
-4.40 |
25,119 |
2,511,886 |
|
-4.35 |
22,387 |
2,238,721 |
|
-4.01 |
10,233 |
1,023,293 |
Mass-loss rates for 21 Wolf-Rayet stars
https://academic.oup.com/mnras/article/196/2/101/963387
MNRAS, 196, 101-110, 1981
|
Star |
Type |
Annual Loss |
Years/Solar Mass |
Years/100 Solar Mass |
|
|
|
|
|
|
|
HD-190918 |
WN4+091 |
0.000019 |
52,632 |
5,263,158 |
|
HD-4004 |
WN5 |
0.000025 |
40,000 |
4,000,000 |
|
HD-50896 |
WN5 |
0.000033 |
30,303 |
3,030,303 |
|
HD-193077 |
WN5 |
0.000017 |
58,824 |
5,882,353 |
|
HD-193576 |
WN5+06 |
0.000018 |
55,556 |
5,555,556 |
|
MR-111(AS422) |
WN5/WC5 |
0.000015 |
66,667 |
6,666,667 |
|
HD-165688 |
WN6 |
0.00003 |
33,333 |
3,333,333 |
|
HD-191765 |
WN6 |
0.000033 |
30,303 |
3,030,303 |
|
HD-192163 |
WN6 |
0.000023 |
43,478 |
4,347,826 |
|
HD-92740 |
WN7 |
0.000038 |
26,316 |
2,631,579 |
|
HD-93131 |
WN7 |
0.000034 |
29,412 |
2,941,176 |
|
HD-93162 |
WN7 |
0.000034 |
29,412 |
2,941,176 |
|
HD-151932 |
WN7 |
0.000039 |
25,641 |
2,564,103 |
|
BAC-209 |
WN8 |
0.00002 |
50,000 |
5,000,000 |
|
AS-374 |
WN8 |
0.000051 |
19,608 |
1,960,784 |
|
HD-165763 |
WC5 |
0.000043 |
23,256 |
2,325,581 |
|
MR-112 |
WC5 |
0.000032 |
31,250 |
3,125,000 |
|
HD-113904 |
WC6+09.51 |
0.000034 |
29,412 |
2,941,176 |
|
HD-152270 |
WC7+05 |
0.000049 |
20,408 |
2,040,816 |
|
HD-68273 |
WC8+091 |
0.000059 |
16,949 |
1,694,915 |
|
HD-192103 |
WC8 |
0.000027 |
37,037 |
3,703,704 |
Mass-loss rates of Wolf–Rayet stars
https://ui.adsabs.harvard.edu/scan/manifest/2000A%26A...360..227N?art=true
Astronomy & Astrophysics, 360, 227–244 (2000)
|
Current Mass |
Solar Masses |
Lifespan |
Current Mass |
Solar Masses |
Lifespan |
|
Sun=1 |
Lost Per Year |
(Years) |
Sun=1 |
Lost Per Year |
(Years) |
|
8 |
0.0000039 |
2,051,282 |
13.4 |
0.000024 |
558,333 |
|
10.3 |
0.000012 |
858,333 |
13.4 |
0.000017 |
788,235 |
|
10.3 |
0.000011 |
936,364 |
15.8 |
0.000025 |
632,000 |
|
18.2 |
0.000023 |
791,304 |
13.4 |
0.0000295 |
454,237 |
|
10.6 |
0.00001 |
1,060,000 |
18.1 |
0.000063 |
287,302 |
|
10.2 |
0.0000068 |
1,500,000 |
7.2 |
0.0000108 |
666,667 |
|
9.6 |
0.000012 |
800,000 |
13 |
0.0000244 |
532,787 |
|
9.6 |
0.0000129 |
744,186 |
10.5 |
0.000015 |
700,000 |
|
15.2 |
0.000024 |
633,333 |
9.2 |
0.000015 |
613,333 |
|
13.1 |
0.0000181 |
723,757 |
9.2 |
0.0000232 |
396,552 |
|
9.6 |
0.000017 |
564,706 |
9.2 |
0.000016 |
575,000 |
|
9.2 |
0.000011 |
836,364 |
8.1 |
0.0000237 |
341,772 |
|
9.1 |
0.0000188 |
484,043 |
9.2 |
0.000024 |
383,333 |
|
9.5 |
0.0000128 |
742,188 |
7.6 |
0.0000114 |
666,667 |
|
10.3 |
0.0000215 |
479,070 |
9.2 |
0.000011 |
836,364 |