<p>The distance between Sirius A and B is between 8 and 31.5 AU and even when Sirius A becomes a red giant it  will be still above 6 AU. Such distance is too large and does not allow Sirius B to accrete significant mass, almost all mass lost by Sirius A as a red giant and later AGB will escape into space. Sirius B may become a recurrent nova due to some accretion, but will not gain enough mass to explode as supernova, it will hardly gain even 0.05-0.1 solar masses.</p>

CC BY-SA 4.0
2019-10-31T08:35:06.183Z
Could you point me to where you got your very definite upper limit of 0.05-0.1 solar masses of accreted material.
ProfRob
CC BY-SA 4.0
2021-01-07T12:08:01.227Z
Distance between two stars is currently between 8 and 31.5 AU even when Sirius Abecomes a red giant it will still be above 6 AU maybe even more because much mass will be lost into space. At 6 AU the white dwarf will accrete some mass but more than around 0.1 solar masses seems practically impossible while at least 0.3 is needed for supernova. Accretion may cause recurrent nova due to nuclear synthesis in falling gas.
Vladislav Peichev
CC BY-SA 4.0
2021-01-07T12:38:09.543Z
That is what my answer says. What I was asking was where you got the 0.05-0.1 solar masses number.
ProfRob
CC BY-SA 4.0
2021-06-30T11:00:24.973Z
This is an estimate, it may accrete a bit more but not much because at 6AU distance its gravity will not be able to hold much gas ejected from red giant or AGB primary. Sirius A should lose around 1.4 Sun masses after leaving the main sequence before forming a white dwarf. Because of the relatively large distance between the components it is highly unlikely that Sirius B will accrete more than 5-10% of the ejected gas and will stay far below Chandrasekar limit. It will be well outside Sirius A's Roche globe.
Vladislav Peichev
CC BY-SA 4.0
2019-02-20T14:45:39.283Z
2019-02-20T14:45:39.283Z
Vladislav Peichev
<p>Sirius b is 1.02 solar masses and is a carbon-oxygen white dwarf. The critical mass depends on its composition, an iron composition white dwarf may have a critical mass of as low as 1.0667 solar masses, see column seven of  the last row of table 3 in <a href="https://iopscience.iop.org/article/10.1088/1674-4527/17/6/61/meta" rel="nofollow noreferrer">this paper</a>. They get lower than the usual values through considering inverse beta decay (proton plus electron combine to make a neutron) also called neutronization. It’s a difficult calculation.</p>

<p>See also stack exchange comment here</p>

<ul>
<li><a href="https://physics.stackexchange.com/questions/345282/why-dont-electrons-and-protons-in-a-white-dwarf-combine-before-the-electrons-be">Why don't electrons and protons in a white dwarf combine before the electrons become ultrarelativistic?</a></li>
</ul>

<p>Anyway with that paper’s suggested correction, again using their table 3, it’s 1.3846 for oxygen and 1.3916 for carbon white dwarfs. Sirius b is still well below critical mass.
When that does happen, Sirius b is probably too far away to accumulated enough gas from it to go supernova and anyway all the stars are moving around the galaxy, chances are that Sirius is a vast distance from us before this can happen, see <a href="https://astronomy.stackexchange.com/a/20124/11432">Rob Jeffries' answer</a></p>

<p>There is another possibility, a sub-Chandrasekar white dwarf. This is a recent idea that it’s possible for a lighter white dwarf to go supernova without reaching the Chandrasekhar limit, making a less energetic supernova.
According to <a href="http://lclavelli.people.ua.edu/uploads/9/5/0/7/95076160/1609.02742r.pdf" rel="nofollow noreferrer">this paper</a> there is some statistical evidence that there may be fewer white dwarfs of mass of 1.1 solar masses and higher than you’d expect from the predicted range of birth masses, suggesting that maybe some of them go supernova as they cool down.
It's unlikely to apply to Sirius b though.</p>

<blockquote>
  <p>"Sirius b, the right-most magenta diamond, is unlikely to produce a supernova unless the critical density is significantly lower than the value taken in fig. 3. In this improbable case many of the high mass dwarfs from ref. [16] would have to be undergoing significant accretion in order to survive to the measured ages." <a href="http://lclavelli.people.ua.edu/uploads/9/5/0/7/95076160/1609.02742r.pdf" rel="nofollow noreferrer">Degeneracy Breakdown as a Source of Supernovae Ia</a></p>
</blockquote>

CC BY-SA 4.0
2019-06-27T12:55:29.577Z
2019-06-27T12:55:29.577Z
Robert Walker
<p><a href="https://i.sstatic.net/IPtSz.jpg" rel="nofollow noreferrer"><img src="https://i.sstatic.net/IPtSz.jpg" alt="accretion Sirius A - B"></a></p>

<p>It is certainly possible, see the picture.</p>

CC BY-SA 4.0
2019-07-03T05:33:03.950Z
2019-07-03T05:54:50.310Z
2019-07-03T05:54:50.310Z
Silver Surfer
<p>Will Sirius B start accreting? Yes, it is doing so now. Sirius A will have a wind and some of that wind will be captured by the white dwarf.</p>

<p>The effectiveness of wind capture is a strong function of relative wind speed. An analytic approximation to the accretion rate, known as <a href="https://en.m.wikipedia.org/wiki/Bondi_accretion" rel="nofollow noreferrer">Bondi-Hoyle accretion</a>, goes as the inverse cube of the relative speed. In its present evolutionary state, the mass loss from Sirius A will be relatively weak (like the Sun) and relatively fast (like the Sun). This disfavours any significant accretion by the white dwarf.</p>

<p>However, in the later stages of its life, Sirius A will swell to become an asymptotic giant star. The envelopes of such stars are gradually (on timescales of millions of years) blown away quite slowly by a dusty wind. If Sirius A is around 2 solar masses now, it will lose about 1.4 solar masses during this phase at speeds of only 10-20 km/s. </p>

<p>Only <em>a fraction</em> of this mass may be accreted by the white dwarf, because the separation between the stars is still large at 25 AU (and will become larger as mass is lost from the system) compared with the likely terminal size of Sirius A (probably of order 2 au). If you look at the <a href="https://en.m.wikipedia.org/wiki/Roche_lobe" rel="nofollow noreferrer">likely Roche lobe size</a>, then Roche lobe overflow would require A to reach about 40% of the separation, which isn't going to happen. Exactly what fraction <em>is</em> captured by the less efficient wind accretion process (the majority will likely disappear into space <em>and</em> widen the orbit) depends strongly on the wind speed, which is hard to predict. </p>

<p>Even if Sirius B could accrete the 0.35-0.4 solar masses (I think that is unlikely, but lack the wherewithal to do the hydrodynamic simulation) it needs to become unstable, it is not clear if that mass will "stick". A build up of hydrogen-rich material can ignite and explode in a nova (not supernova) on the surface of a white dwarf, causing mass loss!</p>

<p>Finally, when will this happen? Well Sirius is probably about 300 million years old now and has another perhaps 500 million years before it starts to evolve in the way I described. It will be nowhere near the Sun then.</p>

CC BY-SA 4.0
2019-06-27T20:54:00.937Z
It's also worth noting that as Sirius A loses mass that escapes to beyond the radius of the Sirius B orbit, the Sirius A-B separation will increase proportionately. While not a huge effect, it's still significant.
Mark Olson
CC BY-SA 4.0
2017-02-22T08:44:33.700Z
2019-09-03T11:44:23.940Z
2019-09-03T11:44:23.940Z
ProfRob
<p>Sirius B is a massive white dwarf of 1 Solar mass, orbiting at about 25 AU distance from the 2 Solar mass Sirius A. As it evolves and expands, will the A star start shedding matter to the white dwarf, and when will this start happening? Will the Sun be at a safe distance when/if it does happen, or is Sirius our doom?</p>

<supernova><binary-star><white-dwarf>
Will Sirius B start accreting from A and become a supernova type Ia?
LocalFluff
# Will Sirius B start accreting from A and become a supernova type Ia?

(Asked by: username_0 on 2017-02-22)

Sirius B is a massive white dwarf of 1 Solar mass, orbiting at about 25 AU distance from the 2 Solar mass Sirius A. As it evolves and expands, will the A star start shedding matter to the white dwarf, and when will this start happening? Will the Sun be at a safe distance when/if it does happen, or is Sirius our doom?

**Tags:** supernova, binary-star, white-dwarf

---

## 4 answers

### Answer by username_2 on 2017-02-22. Score: 17 | Accepted answer

Will Sirius B start accreting? Yes, it is doing so now. Sirius A will have a wind and some of that wind will be captured by the white dwarf.

The effectiveness of wind capture is a strong function of relative wind speed. An analytic approximation to the accretion rate, known as [Bondi-Hoyle accretion](https://en.m.wikipedia.org/wiki/Bondi_accretion), goes as the inverse cube of the relative speed. In its present evolutionary state, the mass loss from Sirius A will be relatively weak (like the Sun) and relatively fast (like the Sun). This disfavours any significant accretion by the white dwarf.

However, in the later stages of its life, Sirius A will swell to become an asymptotic giant star. The envelopes of such stars are gradually (on timescales of millions of years) blown away quite slowly by a dusty wind. If Sirius A is around 2 solar masses now, it will lose about 1.4 solar masses during this phase at speeds of only 10-20 km/s.

Only *a fraction* of this mass may be accreted by the white dwarf, because the separation between the stars is still large at 25 AU (and will become larger as mass is lost from the system) compared with the likely terminal size of Sirius A (probably of order 2 au). If you look at the [likely Roche lobe size](https://en.m.wikipedia.org/wiki/Roche_lobe), then Roche lobe overflow would require A to reach about 40% of the separation, which isn't going to happen. Exactly what fraction *is* captured by the less efficient wind accretion process (the majority will likely disappear into space *and* widen the orbit) depends strongly on the wind speed, which is hard to predict.

Even if Sirius B could accrete the 0.35-0.4 solar masses (I think that is unlikely, but lack the wherewithal to do the hydrodynamic simulation) it needs to become unstable, it is not clear if that mass will "stick". A build up of hydrogen-rich material can ignite and explode in a nova (not supernova) on the surface of a white dwarf, causing mass loss!

Finally, when will this happen? Well Sirius is probably about 300 million years old now and has another perhaps 500 million years before it starts to evolve in the way I described. It will be nowhere near the Sun then.

> **Comments:**
> **username_5**: It's also worth noting that as Sirius A loses mass that escapes to beyond the radius of the Sirius B orbit, the Sirius A-B separation will increase proportionately. While not a huge effect, it's still significant.  

---

### Answer by username_1 on 2019-02-20. Score: 6

The distance between Sirius A and B is between 8 and 31.5 AU and even when Sirius A becomes a red giant it will be still above 6 AU. Such distance is too large and does not allow Sirius B to accrete significant mass, almost all mass lost by Sirius A as a red giant and later AGB will escape into space. Sirius B may become a recurrent nova due to some accretion, but will not gain enough mass to explode as supernova, it will hardly gain even 0.05-0.1 solar masses.

> **Comments:**
> **username_2**: Could you point me to where you got your very definite upper limit of 0.05-0.1 solar masses of accreted material.  
> **username_1**: Distance between two stars is currently between 8 and 31.5 AU even when Sirius Abecomes a red giant it will still be above 6 AU maybe even more because much mass will be lost into space. At 6 AU the white dwarf will accrete some mass but more than around 0.1 solar masses seems practically impossible while at least 0.3 is needed for supernova. Accretion may cause recurrent nova due to nuclear synthesis in falling gas.  
> **username_2**: That is what my answer says. What I was asking was where you got the 0.05-0.1 solar masses number.  
> **username_1**: This is an estimate, it may accrete a bit more but not much because at 6AU distance its gravity will not be able to hold much gas ejected from red giant or AGB primary. Sirius A should lose around 1.4 Sun masses after leaving the main sequence before forming a white dwarf. Because of the relatively large distance between the components it is highly unlikely that Sirius B will accrete more than 5-10% of the ejected gas and will stay far below Chandrasekar limit. It will be well outside Sirius A's Roche globe.  

---

### Answer by username_3 on 2019-06-27. Score: 1

Sirius b is 1.02 solar masses and is a carbon-oxygen white dwarf. The critical mass depends on its composition, an iron composition white dwarf may have a critical mass of as low as 1.0667 solar masses, see column seven of the last row of table 3 in [this paper](https://iopscience.iop.org/article/10.1088/1674-4527/17/6/61/meta). They get lower than the usual values through considering inverse beta decay (proton plus electron combine to make a neutron) also called neutronization. It’s a difficult calculation.

See also stack exchange comment here

* [Why don't electrons and protons in a white dwarf combine before the electrons become ultrarelativistic?](https://physics.stackexchange.com/questions/345282/why-dont-electrons-and-protons-in-a-white-dwarf-combine-before-the-electrons-be)

Anyway with that paper’s suggested correction, again using their table 3, it’s 1.3846 for oxygen and 1.3916 for carbon white dwarfs. Sirius b is still well below critical mass.
When that does happen, Sirius b is probably too far away to accumulated enough gas from it to go supernova and anyway all the stars are moving around the galaxy, chances are that Sirius is a vast distance from us before this can happen, see [Rob Jeffries' answer](https://astronomy.stackexchange.com/a/20124/11432)

There is another possibility, a sub-Chandrasekar white dwarf. This is a recent idea that it’s possible for a lighter white dwarf to go supernova without reaching the Chandrasekhar limit, making a less energetic supernova.
According to [this paper](http://lclavelli.people.ua.edu/uploads/9/5/0/7/95076160/1609.02742r.pdf) there is some statistical evidence that there may be fewer white dwarfs of mass of 1.1 solar masses and higher than you’d expect from the predicted range of birth masses, suggesting that maybe some of them go supernova as they cool down.
It's unlikely to apply to Sirius b though.

> "Sirius b, the right-most magenta diamond, is unlikely to produce a supernova unless the critical density is significantly lower than the value taken in fig. 3. In this improbable case many of the high mass dwarfs from ref. [16] would have to be undergoing significant accretion in order to survive to the measured ages." [Degeneracy Breakdown as a Source of Supernovae Ia](http://lclavelli.people.ua.edu/uploads/9/5/0/7/95076160/1609.02742r.pdf)


---

### Answer by username_4 on 2019-07-03. Score: -1

[![accretion Sirius A - B](https://i.sstatic.net/IPtSz.jpg)](https://i.sstatic.net/IPtSz.jpg)

It is certainly possible, see the picture.


---

