astronomy

V419 Cephei

V419 Cephei is a astronomy topic covered in the lgStudy science library. This page brings together a partial reference excerpt, illustrations, worked examples, real-world applications and a short study plan, so you can understand V419 Cephei rather than just read about it. In short: V419 Cephei (BD+59°2342 or HIP 104719) is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89. Distance The Hipparcos-measured parallax of 0.63±0.29 mas is not well-constrained to evaluate its distance.

Key takeaways

V419 Cephei belongs to astronomy; place it in that map before memorising details.
Learn the definition first, then one example that makes the definition concrete.
Connect V419 Cephei to a quantity you can measure, compute or draw — that is where exam questions come from.
Reproduce the core statement of V419 Cephei from memory before moving on to harder problems.

Reference excerpt

V419 Cephei (BD+59°2342 or HIP 104719) is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.

Distance The Hipparcos-measured parallax of 0.63±0.29 mas is not well-constrained to evaluate its distance. Based on kinematic analysis, its most likely distance is 1,085±320 parsecs, equal to 3,540±1,035 light years. The Gaia Data Release 2 parallax of 1.0342±0.1022 mas is consistent with this distance. It is a member of the stellar association Cepheus OB2-A.

Characteristics V419 Cephei is a red supergiant of spectral type M2 Ib with an effective temperature around 3,700 K and an estimated radius of 533 R☉. The K-band angular diameter measurements equal 5.90 ± 0.70 milliarcseconds, which leads to a figure not much higher, although the uncertainty in its distance must also be taken into account. If placed at the Sun's location, it would engulf the orbits of Mercury, Venus, Earth, Mars, and roughly half of the asteroid belt. Published values for the mass of V419 Cephei vary from around 5 M☉ to over 16 M☉, above the limit beyond which stars end their lives as supernovae. The life of such massive stars is very short. Despite its advanced evolutionary state, V419 Cephei is only 10 million years old. The variability of the brightness of the star was discovered when the Hipparcos data was analyzed. It was given its variable star designation, V419 Cephei, in 1999. Billed as an irregular variable star of type LC, V419 Cephei's brightness varies between magnitudes 6.54 and 6.89 with no apparent periodicity.

References

Illustrations

Worked examples

Example 1 — a first encounter with V419 Cephei

Start with the simplest possible case. Write down what V419 Cephei claims or describes in one sentence, then invent the smallest concrete situation in which that sentence is true. In astronomy, the smallest case is usually a single object, a single equation or a single measurement. Check that every symbol or term in your sentence has a meaning in that case.

Example 2 — changing one variable

Take the situation from Example 1 and change exactly one quantity: double it, halve it, or set it to zero. Predict what should happen to V419 Cephei before you calculate. Comparing your prediction with the result is the fastest way to find out whether you understand the idea or only the words.

Example 3 — an exam-style question

Typical questions about V419 Cephei ask you to (a) state it precisely, (b) apply it to given data, and (c) explain a limitation. Practise writing all three answers in under five minutes; the third part is what separates a full-mark answer from an average one.

Applications of V419 Cephei

In research: V419 Cephei appears in astronomy research whenever the underlying quantities have to be modelled precisely. Papers usually cite it as a starting assumption and then explore where it breaks down.
In technology and industry: Engineering practice reuses V419 Cephei in design rules, simulations and safety margins. Knowing the idea lets you read a specification sheet and understand why the numbers look the way they do.
In the classroom: V419 Cephei is common in secondary-school and first-year university syllabi. It links to neighbouring topics Cepheus (constellation), Durchmusterung objects, Henry Draper Catalogue objects, so understanding it makes those chapters shorter.
In everyday life: Look for V419 Cephei outside the textbook — in sport, cooking, traffic, electronics or the sky above you. An example you found yourself is remembered far longer than one you were given.

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How to study V419 Cephei in 20 minutes

Read the reference excerpt below once, without taking notes.
Close the page and write down what V419 Cephei means in your own words.
Compare your version with the excerpt and mark what you missed.
Work through the three examples above with pen and paper.
Explain V419 Cephei out loud to somebody else — or to Teacher Smith in the lgStudy chat.

Frequently asked questions

What is V419 Cephei in simple terms?

V419 Cephei (BD+59°2342 or HIP 104719) is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89. Distance The Hipparcos-measured parallax of 0.63±0.29 mas is not well-constrained to evaluate its distance.

Why does V419 Cephei matter?

Because it connects several astronomy ideas at once: it gives you a definition you can apply, a quantity you can calculate, and a way to check whether a result is plausible.

How should I study V419 Cephei?

Read the excerpt, restate it from memory, then work through the examples and applications listed on this page. The five-step study plan above takes about twenty minutes.

What does this page cover?

It gives you a compact reference excerpt plus original lgStudy explanations, examples, applications and study material on V419 Cephei.